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ILIESI Institute Lessico Intellettuale Europeo e Storia delle idee
National Research Council
Villa Mirafiori
Via Carlo Fea 2
00161 Roma
Tel. +39 06-86320517/27
Fax +39 06-49917215
ACTIVITIES | Lines of Research | Current
Migration, multilingualism and transmission of knowledge in the Mediterranean area
Together with other initiatives and research activities promoted by the Interior Ministry, the National Academy of Lincei, the Institut of Catalan Studies of Barcelona and the University of Valencia and Lerida, the project aims to examine the relationship between migration and cultural transfers in the Mediterranean area. In particular, it intends to examine the development of plurilingualism and the phases of movement of certain literary works, in order to reconstruct the evolution of such processes and to highlight common characteristics and variations in different historical periods. The main topics of the research project are: 1) the phenomena about mobility and transmission of culture in Italy and euro-Mediterranean area in the contemporary period; 2) the phenomena about mobility and multilingualism in Italy and euro-Mediterranean area, in the past and in the present, with particular reference to the areas of the Crown of Aragon and the Crown of Spain in medieval and modern times; 3) the circulation of books and knowledge between Europe and the New World, with particular reference to the work "Mexican Treasury", published by the Accademia dei Lincei in 1651. Scientific coordinator: Maria Eugenia Cadeddu
Philosophical thought in the ancient world: texts and studies
The main research activities are: (a) the history of ancient philosophy based on the analysis of the texts, particularly the fifth and fourth centuries BC, and the reconstruction of their reception and fortune in late antiquity; (b) the culture and the lexicon of the pre-Greek and non-Greek civilizations of the Ancient Near East; (c) the critical edition and interpretation of largely unpublished philosophical texts of Greek and Roman authors kept in Herculaneum papyri. The project is divided into three areas: Greek philosophy, which brings together the skills of F. Alesse and Luca Simeoni; Ancient Near East, which gathers the skills of S. Chiodi; Herculaneum Papyrology, which gathers the expertise of G. Ranocchia and M. Alessandrelli. The three areas are distinct for research methodologies but united by historical documentary background, from skills of the researchers taking part and especially from the scientific purposes. Scientific coordinator: Francesca Alesse
SATURN - Histories of ideas and cultures: archives, texts, vocabularies and terminology
Activities under project cover all the thematics and the time period which is traditionally studied by the ILIESI research: the history of philosophical and scientific terminology, the implementation of digital archives, seminars and conferences related to history of scientific and philosophical ideas, and their implications on the linguistic and lexical level, including the development of multilingual dictionaries that make possible access to archives and databases. The project takes inspiration both of consolidated activities of the ILIESI (history of ideas as the history of philosophical terminology documented in the texts), as the most recent work on the implementation of digital archives and databases; also it provides for the development of skills related to the publication of editorial series and periodicals both in digital form, as in paper form. The time span of the research is very broad, ranging from studies devoted to the ancient Near East, for the reconstruction in historical comparative perspective of the intellectual world, the study of classical antiquity, with particular attention devoted to practical philosophy and semantics Aristotelian, until the Hellenistic scientific tradition, for which studies are planned on astronomy of Eudoxus of Cnidus, the Renaissance and modern studies in their relationship with the ancient and medieval tradition; the latter a decisive period for European culture, the consequences of which reach up to today. Scientific coordinator: Roberto Palaia
History of ideas and research methodologies
The main research activities concern: the development of studies and research of individual interest in a free theme in the various fields of competence of the Institute; analysis and development of specific methodologies to support historical-philosophical, historical-scientific, philological, linguistic and digital humanistic research. The project formalizes in the structure of a project the research activities that researchers and technologists develop outside the formally constituted and funded projects, in which the scientific management of the Institute is divided. Responsible: Eugenio Canone


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Obagi Gentle Rejuvenation is a soothing skin care system that is specifically designed for sensitive skin. It's also a great routine for anyone who wants to address the early signs of aging, such as fine lines, uneven skin tone and rough texture. If you're new to anti-aging, this skin care line is perfect for you.
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subset: commoncrawl


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TMG celebrated with Planate Management Group to honor its 10-year anniversary. The event was held on November 8, 2017 at the Hilton Alexandria Old Town Hotel. TMG extends a special thanks to Chris Decker, President, and Jonathan Larson, Vice President of Business Operations at Planate for a great event. Congratulations for achieving a remarkable company milestone!
November 16, 2017 by Jacylyn Syfu in TMG News


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BSc Hon (NSW), PhD (NSW)
Professor Pratley graduated with BSc (Hons) from the University of NSW (UNSW) before undertaking PhD studies at UNSW, investigating plant and soil factors affecting the selenium nutrition of grazing livestock.
Professor Pratley took up an academic position at Wagga Wagga Agricultural College (now Charles Sturt University) in 1972 and since then has taught courses in agronomy and related areas and has published widely in conservation farming, weed management, herbicide resistance and allelopathy. He was Foundation Dean of Science and Agriculture at Charles Sturt University from 1990 until 2006.
Professor Pratley is Secretary of the Australian Council of Deans of Agriculture. He is a former President of the Australian Society of Agronomy and former Vice President of the International Allelopathy Society. He has served on the Boards of the Cooperative Research Centres of Viticulture, Sustainable Rice Production, Weed Management Systems and Plant Based Management of Dryland Salinity. He is a member of the Research Committee of the Australian Farm Institute and of the NSW Primary Industries Minister's Science Council.
Stanton RA, Pratley JE, Hudson D, Dill GM (2008). A risk calculator for glyphosate resistance in Lolium rigidum (Gaud .). Pest Management Science 64 (2).
Pratley JE, Broster JC and Michael P (2008). Evaluation of barnyard grass (Echinochloa spp) in Australian rice crops . Australian Journal of Agricultural Research (accepted for publication).
Wu H, Pratley J, Lemerle D, An M and Liu DL (2007). Modern genomic approaches to improving allelopathic capability in wheat (Triticum aestivum L). Allelopathy Journal 19, 97-107.
Bruce SE, Kirkegaard JA, Pratley J, Howe G (2006). Growth suppression of canola through wheat stubble I. Separating physical and biochemical causes in the field. Plant and Soil 281 (1-2), 203-218.
Broster JC and Pratley JE (2006). A decade of monitoring herbicide resistance in Lolium rigidum in Australia. Australian Journal of Experimental Agriculture 46 (9), 1151-1160.


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Southern Gas Association Safety Awards are a means by which companies recognize performance. These awards are provided to member companies to stimulate interest in and add incentive to safety programs.
If you would like to nominate a candidate, please follow one of the links below to fill out the appropriate online application form:Meritorious AwardHumanitarian AwardSponsored by the SGA Employee Safety and Health Committee
The Meritorious winner will be formally announced and awarded at Natural Gas Connect on July 15-17, 2019, in San Antonio, Texas. The Humanitarian Achievement Award is presented on a rolling basis.
If you have any questions, please contact Linda Todd or call 972-620-4013.
Charles Viviano, Boardwalk PipelinesMike Bates, Tennessee Gas PipelineColby Harmon, Tennessee Gas Pipeline/Kinder MorganRyan Williams, Middle Tennessee Natural Gas Utility District
Darrin Carpenter, Kinder MorganJerry Pruitt, Atmos Energy CorporationTim Bowles, Louisville Gas & Electric CompanyTina Revak, Louisville Gas & Electric Company
Tim Martin, Atmos Energy CorporationJoey Hurst, Atmos Energy CorporationJason Price, ONE Gas, Inc./Kansas Gas ServiceKyle Hoeffner, ONE Gas, Inc./Kansas Gas ServiceDustin Ehlrich, ONE Gas, Inc./Kansas Gas Service
Alina Alamo, TECO Peoples Gas/EmeraSteve Arden, CenterPoint EnergyJames Chastain, CenterPoint EnergyPaul Day, Kinder MorganMcKinley Coleman, Atmos Energy Corporation
Carol Donnellan, CenterPoint EnergyPeyton Franco, Tennessee Gas PipelineLarry Juday, CenterPoint EnergyGregory Lanette, CenterPoint EnergyMark Childers, CenterPoint Energy
Southern Gas Association 3030 LBJ Freeway, Suite 1500, Dallas, TX 75234 Phone: 972-620-8505 | Fax: 972-620-1613 Email: firstname.lastname@example.com Hours: 8:00 a.m. - 5:00 p.m. CST
For more than a century, SGA has been focused on growing individuals and advancing the industry by linking people, ideas and information. Representing the industry as a whole from drill bit to burner tip, SGA's membership comprises 200 businesses across the distribution, pipeline and gas supply marketing sectors as well as more than 300 industry partners who serve the industry as vendors, suppliers and consultants.


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This dashboard page helps your to visualize the relative weight of each specialty in your hospital/clinic activities.
- The vertical axis is based on the Cost-Weight per Stay.
- The horizontal axis is based on the Nb of Stays.
- You have one bubble per Specialty, sized by Total Cost-Weight.
Specialties at the top left of the chart are specialties with low number of stays but with high Cost-Weight per Stay.
Specialties at the bottom right of the chart are specialties with high number of stays but with low Cost-Weight per Stay.
For each specialty, the line shows the evolution across years.
Select Year Range
This data visualization comes with a filter on the Date value. This feature enables you to focus on the range of years you are interested in.
Filter your data
This data visualization comes with four top filters:
In your Patient Record + DRG dashboard, you will be able to filter on:
- SpecialtyMedical Specialty
- ServiceService
- DoctorDoctor
- Discharge ModeDischarge Mode


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Meccano Junior Advanced Toolbox Set, Multicolor
$17.49 $34.99
Challenge the boundaries of your child's imagination as they discover elements of real engineering with the Meccano Junior Advanced Toolbox. Helps develop early logic & hand motor skills Create 8 different models, including a dump truck, crane, excavator & windmill Convenient storage tool box for easy transport Easy to follow step-by-step instructions are provided so little hands can piece together large connecting parts with snap-on clipping connectors & add-on wheels 7.87H x 11.61W x 6.5D Age: 5 years & up 88-piece Size: One Size. Color: Multicolor. Gender: Male. Age Group: Kids.
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* This offer may contain time-sensitive information and offers. Please check with Kohl's to confirm actual price & availability.
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Mark writes:
Andrew Smith has won an award on Crossrail Anglia for his impact on health and safety.
Sarah Brock from Crossrail presented him with his award on site at Ilford on 5 April. The award is for his contribution to improving health and safety awareness on site, including putting in close call cards and suggesting improvements. He also helps out anyone who needs support, no matter if they are VGC or from another company: for example, he taught some of the COSS (controllers of site safety) how to use the Sentinel app to check workers' smartcards.
Andrew is a site supervisor, working on the stations upgrade for Crossrail for our client Costain. He is currently involved in the platform extension at Ilford station. He's really good: when I first interviewed him it was obvious that he has the right attitude to be a real asset to VGC and our clients.


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What Happened To The Later Members?
After Rollermania began to calm down the Rollers changed their line-up. Alan decided he was too old to be in the group and was replaced in 1976. Many fans in the UK were heartbroken and to this day refuse to even recognize the later members of the group. But there were some fans who accepted them. So I've decided to put something about them here. I was going to leave them out, because to be truthful, as far as I'm concerned the BCR are the classic five only! But for those who think differently and would like to know what became of the later members you can find out a bit more here.


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Search the Community
Showing results for tags 'xbox one'.
Found 16 results
Fanatec CSL Elite wheel with Thrustmaster TP3A Pro pedals.
georgemate posted a topic in Sim Racing DiscussionSimple question! Can I use a Fanatec CSL Elite wheel with Thrustmaster TP3A Pro pedals on Xbox one X ? Any advise welcome!
Xbox One, PS4, PC & PS3 Motion Simulator available
Jason187781 posted a topic in Sim Racing Rigs / CockpitHi All, I have been under the radar now for months busy beavering away on a Motion simulator that works with Next Gen consoles and PC. Well I am over the moon to be able to say I have done it! I am now putting myself out there for the world to see and answer as many questions as I can with a view to making these available as soon as possible. I'm not interested in being the next bill gates, rather I want to build and sell these as my day job and make it possible for everyone to enjoy one. This is my ( in progress ) website: http://www.caniseng.com/ And my all important Indygogo for funding setup: https://www.indiegogo.com/projects/motion-simulator-for-next-generation-consoles/x/13814348#/ Thanks again Jason
Vibration motors on a t3pa pro
Jacks disciple posted a topic in Thrustmaster ModificationsHey guys, I was wondering if any of yall have installed rumble motors onto your peddles? And if so do yall know if I could get this to work on an xbox one? Been wanting to do this for quite some time but. Not sure if I can get it to work on xbox. If any of yall have done this, could you give me some info on how to go about this. Thanks in advance guys.
xbox one Fanatec for Xbox one and F1 2017
prodiver posted a topic in FanatecI am struggling to decide whether Fanatec is the right choice for F1 2017 on Xbox One? I have read alot of reviews and it seems that on Xbox one I will not enjoy the full potential of the wheel especially on F1 2017. I also plan to get Assetto Corsa but would you like to get your thoughts for Fanatec on Xbox One?
SOLD Fanatec ClubSport Wheel Rim GT Forza Motorsport Model: UH RGTF NEW
SuperClyde45 posted a topic in Sim Gear - Buy and SellNEW. OPEN BOX. Will be packed very well. Must Include ISRTV in your offer! This allows me to know that you used this link, which equates to me having lower fees from eBay, which translates to me being able to be more "Negotiable" on your offer. Thank you. http://rover.ebay.com/rover/1/711-53200-19255-0/1?icep_ff3=2&pub=5575378759&campid=5338273189&customid=&icep_item=153038182222&ipn=psmain&icep_vectorid=229466&kwid=902099&mtid=824&kw=lg&toolid=11111 Fanatec ClubSport Wheel Rim GT Forza Motorsport Model: UH RGTF NEW
Gtgmr posted a topic in Sim Gear - Buy and SellHey guys, I have a complete plug and play setup for xbox one. its a thrustmaster tx base, the 599xxevo alcantara wheel, t3pa pro pedals and the thrustmaster shifter. located in Georgia. looking to sell it all together but willing to separate. open to offers! buyer pays shipping
Selling - Logitech G920 + Pedals + G27 Shifter
p4nc4kemix4u posted a topic in Sim Gear - Buy and SellSold
Vintage Endurance Racing Championship
Pracer36 posted a topic in Project CARS 2Hello everyone, Now that Project Cars 2 has come out it seems to be great for doing an endurance racing series. Specifically vintage endurance racing. This series will be run on Xbox and we will use Group C prototypes and Group 5 sports cars for the first season. In future seasons we can switch to a different era of racing if people want to. Races will be held on Saturdays at 7pm eastern US time. The session will open at 7. Qualifying will last 15 minutes and the race will start at 7:15. Normal races will be 2 hours long, special races such as Le Mans and Daytona will be longer. We want to get an equal number of people in prototypes and GT cars. To sign up simply respond to this thread with your gamer tag, the car and class you will be participating in, and the eastern US time that you would prefer normal races to start at. Also we will need one person to volunteer to be the safety car driver and another to be chief steward. Entries will close on October 14th. RULES -Light body contact only, heavy contact will result in penalties -We will have full course cautions and a safety car, during a full course caution cars will line up single file behind the safety car. The drivers involved in the accident must pause and retire from the race during this period. The safety car period will last until the field is gathered up by the safety, even if cars pit. Green flag racing will resume after this and the lead car can only start speeding up after the pace car enters pit lane and there will be no overtaking before start/finish. -If there are two versions of the car you choose, one high downforce and the other low downforce, you can switch cars depending on the track. It is your choice as to which version to use for which track, i.e. you won't be penalized for using a lower downforce car at a high downforce track and vice versa. -You can make as many pitstops as you want and there is no required tire compound you need to use. -Races such as Le Mans and Daytona will offer double points. -There will be no ridiculous blocking. You can use slower traffic to your advantage and other stuff of that nature, as that is one of the things that makes multiclass racing fun. But cutting off a car multiple times on straights will not be allowed. -Causing a crash will be dealt with depending on the incident. -If you are unable to participate in a race you must contact us through the email address I will give all the participants in order to keep everything smooth. Failure to do so the first time will result in a warning, twice will be a 1 race suspension, and three times will result in you being kicked out of the series. -Drivers who constantly get involved in incidents that effect others will be forced to leave the series. Obviously in racing there are incidents, but drivers who cause chaos all the time will not be tolerated. POINTS SYSTEM 1st - 25 points 2nd - 20 points 3rd - 15 points 4th - 12 points 5th - 10 points 6th - 8 points 7th - 7 points 8th - 6 points 9th - 5 points 10th - 4 points 11th - 3 points 12th - 2 points 13th - 1 point 14th - 0 points 15th - 0 points 16th - 0 points
Codemasters F1 2016 using Xbox one.
Sparky996 posted a topic in Sim Racing DiscussionHi Guys & Gals, A question, every time I turn on my Xbox (with F1 2016 disc in it) when I go to a track that I have driven before I get my lap times and data etc. displayed. I want to delete / erase this info and start again ........ how is this done please !!!! .... thanks in advance. Sparky.
Never ending build
JCMgraphics posted a topic in Sim Racing Rigs / CockpitBeen working on this " car " cockpit for my son for a while. I keep changing and adding to it. Started out as a box looking rig with a door to get in. We used to roll it in front of the TV to play but as I was adding more, I decided to mount a TV to it. Gear used: Thrustmaster TMX wheel, T3pa pedals, Th8a shifter, custom handbrake, 42" Samsung TV, Sony/Yamaha 5.1 surround, ACM boards ( aluminum composite material ) and lots of vinyl decals haha. The seat is adjustable and also the steering wheel ( forward and back for people with longer legs ).The going theme is Subaru because we love the cars but also the whole built was base around the STI seat. Next ( already ordered ) is a shift boot for the handbrake and a new shift knob. Tons of hours are spent on this thing. Not as fancy as those pre-fab one but a fun father/son project.
Need advise on what to buy...
Jaspervb96 posted a topic in Getting Started In Sim RacingFor a bit of context: Early 2017 I bought my first wheel (g920) to play FH3 & FM6 on Xbox One, I enjoyed this wheel very much until I started to play nothing else but F1 2017. I sold the Logitech and bought a TM TX Leather edition with the F1 wheel (offcourse). Unfortunately, after 2 months it stopped working and had to send it back to the store (kept my F1 wheel). Since the TX base is known for its fluctuating reliability, and the fact that its design is about 2 years old, I got the TS-XW racer. I have been testing this thing for about 3 weeks, and also decided to return it. (Due to cheap pedals and expensive Sparco wheel which I almost never use) Now, I have a budget of aprox. €650,-. Which will get me a ts-xw, or a entry level Fanetec setup without F1 wheel. Or, again a TX unit and save a lot of money (possibly). Another option is for me to wait what TM is going to release this year. But that might not pay off. What is your advice? Are there any rumours of new TM set's coming? Is Fanetec really worth the investment? Thank you for reading, looking forward to your answers.
SOLD: Fanatec Racing Simulator Obutto Racing cockpit (South Florida, USA)
Gsosa posted a topic in Sim Gear - Buy and SellFor sale I have a complete Fanatec racing simulator with Obutto racing cockpit, compatible with pc, xbox one and ps4 race simulator gaming. All equipment is in "like new" condition, have been lightly used. Still have original boxes for everything except the cockpit and monitor.Obutto R3volution Gaming cockpit-Excellent condition, racing seat is mint. All bolts and accessories included. Was purchased new for $899.99 + shipping.Fanatec clubsport wheel base v2 - $499.95Fanatec CSL steering wheel p1 (for xbox one) - $89.95Fanatec clubsport steering wheel formula black - $199.95Fanatec clubsport pedals v3 - $329.95Fanatec clubsport shifter sq v1.5 - $199.95Dell U2713HMt 27" LED widescreen monitor (discontinued) - $250I want to sell the simulator and cockpit, everything together, not willing to part out. I spent over $2,500 for this set up brand new. Everything is working and in excellent condition. Obutto cockpit is currently on back order. I will let everything go for $1500 obo. This is a steal. Everything is like new.Local pick up in South Florida only. Will not ship. Cash only.Text or call 786 546 6503
T3PA PRO(BRAND NEW NEVER USED) & used Ferrari 599xx eve
Gtgmr posted a topic in Sim Gear - Buy and Sellhey guys, happy holidays! i have a new set of thrust master T3PA PRO pedals that were never used. i bought it to use with my x box then i ended up buying a complete setup from some one so i have not yet used these. i also have a thrust master 599XX EVO alcantara wheel i bought used but haven't used myself. then i have a tx wheel base that is not working. i bought it from someone practically new in the box but it never turned on for me. i did splice off the breakaway usb trying to see if that was the problem(known issue) . if you are electronically inclined you may be able to fix it. Im asking 120 for the pedals, 130 for the wheel and 75 for the tx base as is. please msg me or text me on 3476107976 for questions. price is shipped in the us.
Custom Thrustmaster steering wheels with console comparability
Pracer36 posted a topic in Sim Gear - Buy and SellHi everyone, I have figured out how to build custom steering wheels that connect to your Thrustmaster wheel base and works with the Xbox One and PS4. You simply connect it to the wheel base like a normal thrustmaster wheel. I am going to start making fully custom wheels for people. These wheels will be designed to fit your needs. The only requirements are that the wheels cannot have rotary encoders due to the wheel base not being able to recognize them, console users need to have at least 10 buttons, and there is a max of 13 buttons for console and pc users. If you are interested send me a private message and we can get started on designing and building a wheel that suits you.
Custom Thrustmaster wheels with console compatibility
Pracer36 posted a topic in Sim Racing DiscussionHi everyone, I have figured out how to build custom steering wheels that connect to your Thrustmaster wheel base and works with the Xbox One and PS4. You simply connect it to the wheel base like a normal thrustmaster wheel. I am going to start making fully custom wheels for people. These wheels will be designed to fit your needs. The only requirements are that the wheels cannot have rotary encoders due to the wheel base not being able to recognize them, console users need to have at least 10 buttons, and there is a max of 13 buttons for console and pc users. If you are interested send me a private message and we can get started on designing and building a wheel that suits you.
FS : XCM Maxrace F1 V4 Adapter
obis posted a topic in Sim Gear - Buy and SellFor Sale XCM MaxRace F1 V4 Adapter to convert g27 wheel to xbox one 40 Euros shipping not included from Spain


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Queensberry House B&B
12 Beechgrove, Moffat DG10 9RS, UKFind Out More
Dell Mar
Beechgrove, Moffat DG10 9RS, UKFind Out More
Over Phawhope (NT 182082)
Over Phawhope Bothy, Selkirk, United KingdomFind Out More
Dumcrieff House
Dumcrieff House, Old Carlisle Road, Moffat, United KingdomFind Out More
Hillend Guest Cottage (NT 104046)
Hillend Guest Cottage, Moffat, DG10 9LEFind Out More
Tibbieshiels Inn Camp Site (NT 241206)
Tibbieshiels Inn Camp Site, St Mary's LochFind Out More
Honey Cottage Caravan Park (NT 296163)
Honey Cottage Caravan Park, Hope House, Ettrick Valley, Selkirk, TD7 5HUFind Out More
Hartleap B&B
Hartleap Bed and Breakfast, Yarrow, Selkirk, TD7 5NQFind Out More
Moffat B&B
Moffat B&B, 29 Well Street, Moffat, DG10 9DPFind Out More
Seamore Guest House
Seamore Guest House, Academy Road, Moffat, DG10 9HWFind Out More
The Limetree House Guest House
The Limetree House Guest House, Eastgate, Moffat, DG10 9HWFind Out More
Tushielaw Inn
Tushielaw Inn, Tushielaw, Ettrick Valley, TD7 5HTFind Out More
Woodhead Farmhouse B&B
Woodhead Farmhouse B&B, Old Carlisle Road, Moffat, DG10 9LUFind Out More
Moffat Manor Holiday Park, Beattock
Craigielands Country Park, Beattock, DG10 9REFind Out More
Cauldholm Bed & Breakfast
Cauldholm B&B, Beattock, DG10 9QAFind Out More
The Old Stables Inn
The Old Stables Inn, Main Street, Beattock, DG10 9QXFind Out More
Lochhouse Farm
Lochhouse Farm, Beattock, DG10 9SGFind Out More
Summerlea House Moffat Bed and Breakfast
Summerlea House, Eastgate, Moffat DG10 9AD, United KingdomFind Out More
Gordon Arms Hotel
Gordon Arms Hotel, Selkirk TD7 5LE, United KingdomFind Out More
Hartfell House & The Lime Tree Restaurant
Hartfell House & The Limetree Restaurant, Hartfell Crescent, Moffat DG10 9AL, United KingdomFind Out More
The Old Stables InnFind us
Main Street
Dumcrieff HouseFind us
Old Carlisle Road
Moffat B&BFind us
29 Well Street
A range of produce, accommodation and services are available in Moffat, 1.5 miles north of Beattock. Details from Moffat Tourist Information Centre 01683 220620 or Visit Scotland Dumfries & Galloway, 64 Whitesands, Dumfries, DG1 2RS, 01387 245550. Please note, Moffat is the last town close to the Way where items or provisions can be purchased before reaching Galashiels.
Eating Places
Glen Café, St Mary's Loch, Selkirk, TD7 5LH (NT 237204)
01750 42241
Just across bridge from the Way, Wi-Fi available
Open Easter to end of Oct 10.00-17.00, closed Tuesdays, variable winter opening hours.
Packed Lunch Available.
Hawick 01450 375051
Galashiels 01896 752222
Moffat 01683 220197


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26 Gauge Paneling – 0.48 mm thick. It is a great option to add extra heavy-duty coverage from snowfall, ice, and hail. The extra thickness definitely gives our customers a peace of mind during unforeseen weather. 26 Gauge sheet panels are available on special orders. Restrictions apply.
12 Gauge Tubing – 2-1/4" wide. It comes with a 20 year limited warranty on rust through of framing assuming normal user care and maintenance. See contract for details.
Roof Styles – Upgrade to our residential style roofs; A-Frame Horizontal or A-Frame Vertical
Extra Trusses – Concerned about snow? Add extra trusses to increase your Snow PSI rating.
Larger Braces – Depending on width and height of structure, brace size will vary to keep your building strong and stable.
American Steel Carport's products are engineer certified to meet your state codes (except hunting blinds). Any other requirements such as "extra snow load baring weight and wind load resistance" can be met with engineer certification "upon customer's request". Customized buildings are always welcomed. We also provide generic plans at no extra charge on most standard buildings.
American Steel warrants for a period of 20 years from the date of completion of installation, against rust through on the framing only assuming normal user care and maintenance on 12 gauge materials. This warranty does not apply to 14 gauge materials. Additionally, galvanization extends the life and appearance of your next structure.
Because we understand the hassle of hiring contractors, we install your steel structure at no extra cost to you on your level land. Don't worry, we assist our customers every step of the way.
Stronger Lasts Longer. With the optional wind warranty packages your structure is guaranteed to withstand harsh winds, plain and simple. Wind warranty packages start from 90 mph and up.
Our metal buildings are reinforced with braces on every corner and center of every truss. These braces are put in place to ensure your shelter remains squared and stable for extra strength, while preventing the roof from caving.
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This article has an erratum: [erratum]
Volume 532, August 2011
|Article Number
|Number of page(s)
|Astrophysical processes
|Published online
|14 July 2011
Magnetic coupling of planets and small bodies with a pulsar wind
LUTH, Observatoire de Paris, CNRS, Unviersité Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France
e-mail: email@example.com
2 Observatoire Astronomique, Université de Strasbourg, 11 rue de l'Université, 67000 Strasbourg, France
e-mail: firstname.lastname@example.com
Received: 17 January 2011
Accepted: 25 May 2011
Aims. We investigate the electromagnetic interaction of a relativistic stellar wind with a planet or a smaller body in orbit around the star. This may be relevant to objects orbiting a pulsar that are expected to hold a planetary system, such as PSR B1257+12 and PSR B1620-26, or to pulsars with suspected asteroids or comets.
Methods. We extend the theory of Alfvén wings to relativistic winds.
Results. When the wind is relativistic but slower than the total Alfvén speed, a system of electric currents carried by a stationary Alfvénic structure is driven by the planet or by its surroundings.For an Earth-like planet around a "standard" second pulsar, the associated current can reach the same magnitude as the Goldreich-Julian current that powers the pulsar's magnetosphere.
Key words: plasmas / relativistic processes / methods: analytical / pulsars: general / planets and satellites: dynamical evolution and stability / planet-star interactions
1. Introduction
Precise pulsar timing measurents proved that the pulsars PSR B1257+12 and PSR B1620-26 host planets at distances of the order of an astronomical unit (Wolszczan & Frail 1992; Thorsett et al. 1993). Moreover, accretion discs are expected to form at some phase of the evolution of neutron stars in a binary system, possibly giving birth to second-generation planets. Small bodies such as planetoids, asteroids, or comets may also orbit pulsars and occasionally fall onto them.
Circum-pulsar objects move in the centrifugally driven relativistic pulsar wind. The angular velocity Ω∗ of a rotating neutron star typically is higher than 10 rad s-1. The star behaves like an antenna (Deutsch 1955) emitting a power by magnetic dipole radiation that causes it to lose rotational energy at a rate (1)where MI ≈ (2/5)MR2 is the neutron star's moment of inertia (Lyne & Graham-Smith 1998). This power can be compared to the orbital energy of a pulsar planet. Consider, for example, the case of PSR B1257+12 and its planet "a". Using the data in Tables 1 and 2, we can estimate the moment of inertia to be MI = 1. × 1038 kg m2, the star's rotational energy loss to be Ėrot = −2. × 1027 W, and the planet's orbital energy to be EG = GM∗MP/2a = 4. × 1032 J, where a stands for the planet's semi-major axis. The planet and its environment intercept a fraction higher than or of the order of of this power. This captured power is used to heat the planet, to generate the current system described below, and to work on the planet's motion as described in the accompanying paper (Mottez & Heyvaerts 2011, hereafter MH2). The planet's radius can be inferred from its mass by assuming a terrestrial density (5000 kg m-3). The intercepted power Ėcapt is (2)For planet "a" of PSR B1257+12, we find, Ėcapt = 1.74 × 1018 Watt. If a substantial part of this power goes into planet's motion, an orbital evolution time-scale of about 8 × 106 years may be expected. This is a short time scale by astronomical standards. It scales with the mass MP of the planet as .
In this paper, we examine the interaction of these planets with the magnetized wind of their pulsar and discuss in MH2 the effect of this interaction on the long-term evolution of their orbital elements.
The energy flux carried by the wind of an ordinary star, such as the Sun, is low enough to have but negligible effect on the orbits of its planets. Stellar winds usually are asymptotically super-Alfvénic, by which we mean that they eventually become faster than the total Alfvén speed, which is associated with the modulus of the magnetic field. As a result, the planets are protected from a direct contact with the wind by a bow shock.
Pulsar winds are much different. In a first approximation, oblique rotator pulsars may be regarded as magnetic dipoles rotating at high angular velocity in vacuo, which causes a low frequency and large amplitude electromagnetic wave to be emitted, the wave character of which reveals itself in the wave zone, beyond the light cylinder, of radius r = c/Ω∗. In this zone, magnetic field lines become spiral-shaped and the azimuthal component of the magnetic field decreases as Bφ ~ r-1 while its radial component decreases as Br ~ r-2. The magnetic field becomes mostly azimuthal at large distances and at the equatorial latitudes were the planets are expected to be found. Aligned rotators are essentially rotating unipolar inductors that generate a highly relativistic MHD wind beyond the light cylinder in which the magnetic field also becomes predominantly azimuthal at large distances from the rotation axis. The field components Bφ and Br essentially vary with distance as indicated above, at least near the equatorial plane and when the flow is close to being radial. The power emitted by these objects is also of the order of Ėrot, given by Eq. (1) because the Poynting flux emitted through the light cylinder is comparable for wind or wave emission. We only consider aligned rotators in this paper. Their analysis is simplified because the magnetic field of the wind observed in the planet's frame is close to being time-independent. The origin, acceleration, and structure of pulsar winds are not fully understood. A number of models have been proposed in the literature (Michel 1969; Henriksen & Rayburn 1971; Contopoulos et al. 1999; Michel 2005; Bucciantini et al. 2006). In spite of their diversity, they all conclude that the wind is dominated by the Poynting flux, although observations indicate that they turn into matter-dominated high-energy flows at large distances (Kirk et al. 2009). At distances of the order of an astronomical unit, pulsar winds are expected to still be Poynting-flux-dominated.This means that the electromagnetic energy density ~ , μ0 being the magnetic permeability of vacuum, is much higher than the plasma energy density γ0ρ0c2, γ0 being its Lorentz factor and ρ0 the rest-mass density of this supposedly cold wind. These quantities refer to the observer's frame. In these circumstances, Alfvénic perturbations propagate at a phase velocity close to the speed of light (Eq. (3)). Therefore, although it is highly relativistic, the wind flow may nevertheless be sub-Alfvénic, in the sense defined above. A planet in a Poynting-flux-dominated wind may remain unscreened from the wind by a bow shock and thus enter in direct contact with it.
The interaction of a planet with a sub-Alfvénic plasma flow has been considered for moderately magnetized non-relativistic flows in connection with the interaction of the satellite Io with the plasma and magnetic field present in Jupiter's magnetospheric environment. This interaction is driven by the inductive electromotive field that results from the motion of the satellite across Jupiter's corotational magnetic field and plasma flow. The satellite acts as a (uniformly moving) unipolar inductor. Neubauer (1980) derived a nonlinear theory of this interaction. The Alfvén wing connecting Io and Jupiter is the only explored case of such a structure in the universe up to now, and it has been the object of recent studies concerning its overall structure (Chust et al. 2005; Hess et al. 2010), the possibility of particle acceleration (Hess et al. 2007b, 2009b), and its consequences on the radio emissions (Queinnec & Zarka 1998; Hess et al. 2007a, 2009a). In the present paper, we develop a theory that generalizes some of Neubauer's results to highly magnetized () and relativistic plasma flows with Lorentz factors γ0 ≫ 1, when a planet immersed in the magnetized pulsar wind acts as a unipolar inductor and generates two stationary Alfvénic structures that emerge from the planet and extend far into the wind.
2. A unipolar inductor in the pulsar wind
Let us consider a planet orbiting a pulsar in the relativistic flow of the emitted wind. Different reference frames can be involved in the description of the fluid motion. The frame where the neutron star is at rest is the observer's frame. We denote it by RO. Because the planet velocity is low compared to the wind velocity, we may consider the planet to be at rest with respect to the neutron star, except when discussing the planet's motion. The reference frame RO can then also be regarded as being the planet's rest frame. Quantities observed in this frame are denoted by letters without any superscript, such as ρ or v. The unperturbed wind's instantaneous rest frame in the vicinity of the planet is the "wind's frame" RW. Quantities observed in this frame are denoted by letters with a prime superscript, such as ρ′. An index 0 refers to quantities associated with the unperturbed wind. The unperturbed wind velocity in RO is v0, its associated Lorentz factor is γ0, the unperturbed magnetic field is B0 and the wind's density is ρ0. Because the wind plasma is supposedly cold, this mass density reduces to the (apparent) rest-mass density of particles. In the wind frame RW, the unperturbed wind density is its proper rest-mass density and its magnetic field is . They both differ from ρ0 and B0. In the presence of a perturbation, the instantaneous rest frame of the fluid is not RW, but another rest frame, RF. Quantities observed in this instantaneous rest frame are indicated by a subscript F.
The perturbation generated by the planet in this flow is time-dependent in the wind's frame. Because in the tenuous and highly magnetized pulsar wind the formal Alfvén velocity cA may exceed the speed of light, the derivation of the propagation velocity of Alfvénic perturbations must take into account the displacement current. In the wind's rest frame: (3)If the flow is faster than the Alfvén velocity VA, the planet is preceded by a shock wave that defines a confined area where the flow is strongly modified. But if the flow is sub-Alfvénic, the planet is directly in contact with the wind. In the instantaneous rest frame of the wind plasma we expect, following the MHD approximation, the electric field to vanish. In the planet's rest frame an electromotive field E = −v × B is generated, where B and v are the magnetic field and fluid velocity in the planet's frame.
Using a model pulsar wind, it is possible to make an estimate of the electric field. One of the simplest such models was developed by Michel (1969). It includes the magnetic field and the star's rotation as well as wind particles masses, but neglects the dipole inclination and the gravitation and assumes the wind flow to be radial. The unperturbed magnetic field B0 only has a radial poloidal component and an azimuthal toroidal component . The neglect of the latitudinal component is justified near the equatorial plane and far enough from the inner magnetosphere (Contopoulos et al. 1999). For bodies orbiting near this plane, as circumpulsar planets probably do, this geometrical restriction is unimportant. Other models for steady-state axisymmetric winds have been developed since then (Beskin et al. 1998; Bucciantini et al. 2006). The stationary equations of an axisymmetric perfect MHD flow admit a set of integrals of motion along stream lines, such as the mass flux f and the magnetic flux Ψ, which for cold radial flows and radial poloïdal fields are defined by where all quantities refer to the unperturbed wind as seen in the observer's frame. The MHD approximation E0 + v0 × B0 = 0 and the Faraday equation imply (Mestel 1961) (6)In order to judge whether the planet is in superalfvénic motion with respect to the wind, we should assess whether the modulus of its velocity in the wind's frame, which equals that of the wind in the observer's frame, v0, is faster or slower than the propagation speed in the wind's frame, , defined by Eq. (3). The square of the ratio of these two velocities is given for an asymptotically radial wind by (7)Because the wind is supposedly radial, vanishes. This simplifies Eq. (6), which also shows that at distances much larger than the light cylinder radius,
Input data of the pulsars.
the radial component of the magnetic field can be neglected compared to the azimuthal one. The Alfvén speed cA calculated in the observer's frame is given using Eqs. (4) and (5) to express and ρ0 by (8)The square of the Alfvén speed in the wind's frame is a factor γ0 smaller than the square of the Alfvén speed cA in the observer's frame because and . The latter relation is a result of the vanishing of the electric field in the wind's frame and of the velocity v0 being perpendicular to the azimuthal field. Then (9)where σ0 is the magnetization parameter: (10)In highly relativistic Poynting-flux-dominated outflows, as is expected for pulsar winds, σ0 ≫ 1. The models show that asymptotically the Lorentz factor γ0 approaches and thus (v0/c)2 approaches . From Eq. (9) it is found that to lowest order in an expansion in , the asymptotic value of is . Therefore the pulsar wind remains slower than the total Alfvén speed (3).
Because this result applies at distances much larger than the light cylinder radius, it is essentially valid wherever orbiting planets may be found. We therefore consider that the planets detected around pulsars orbit in a sub-Alfvénic relativistic pulsar wind.
In the numerical computations, we are less subtle and state that at the planetary distances, v0 ~ c and VA ~ c, every time it makes sense. Then, in first approximation, the unipolar inductor electric potential drop U (along the θ axis, i.e. perpendicular to the orbital plane) is (11)Figure 1 provides a representation of the geometric configuration of the unipolar inductor.
Fig. 1
Schematic view of a unipolar inductor.
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The rotation period of the pulsar PSR 1257+12 is P = 0,006s, which corresponds to Ω∗ = 1010 397 rad s-1 and its surface magnetic field is estimated to B∗ ≃ 8.8 × 108 G (Taylor et al. 2000). We assume a star radius R∗ = 10 km and a mass M∗ = 1.4 M⊙ (see Table 1).Data concerning this planet can be read in Table 2. We assumean Earth-like density of 5000 kg m-3. The flux Wb. The semi-major axis, the planetary radius RP = (3MP/4πρP)1/3 and an estimate of U are given for each planet "a", "b", "c" orbiting this pulsar in Tables 2 and 3. Evidently, the inductor electric potential drop U (from pole to pole along the planet) is of the order of 1012 V.
Input data concerning the planets: mass, radius, orbital period, semi-major axis, excentricity.
Electric potential drop and total electric current associated to the Alfvén wing.
For the pulsar PSR 1620-26, the rotation period is P = 0.011s, Ω∗ = 567 rad s-1, the surface magnetic field is estimated to B∗ = 3. × 109 G (Taylor et al. 2000). Still assuming that R∗ = 10 km, we find that Ψ = 3 × 1013 Wb. This pulsar has a white dwarf companion star. The neutron star mass can be estimated to M∗ = 1.35 M⊙ (Thorsett & Arzoumanian 1999; Sigurdsson et al. 2003). The planet is more distant from its star than in the case of PSR 1257+12 but the planetary radius is larger. The resulting potential drop U is still of the same order of magnitude.
We show in Sects. 3 − 5 that a planet in the wind generates two current systems that propagate far in space, forming a so-called Alfvén wing.
3. Equations of special-relativistic ideal MHD
In this section, the equations up to Eq. (23) are general to special relativity, and valid for quantities defined in any inertial reference frame. We use notations without prime and subscript. After Eq. (23), quantities without prime and subscript refer, as in the previous sections, only to the observer's frame RO defined at the beginning of Sect. 2.
A condition for MHD to be valid is that the typical length scale L relevant to the flow be much longer than the particles Larmor radii ρL = γv⊥/ωc, where v⊥ is the typical velocity perpendicular to the magnetic field in the fluid's frame, ωc the gyrofrequency and γ the particle's Lorentz factor in the same frame. The energy of particles in a pulsar wind is a priori very high because the wind's bulk Lorentz factor γ0 may be as high as 105 to 107. If, however, in the wind's frame a significant part of this energy resided in perpendicular motions, particles would very quickly loose it by synchrotron radiation, even in a moderate magnetic field. Therefore, we may consider the pulsar wind particles to have negligible Larmor radii in the rest frame of the wind's bulk flow, so that MHD is applicable on almost any scale.
The fourth component of position in space time is x4 = ct, t being the time measured in seconds in the given reference frame and c the speed of light. Greek indices label four-dimensional coordinates and components and Latin indices label Euclidean three-dimensional ones. The metric tensor of Minkowskian space is diagonal, with components η44 = + 1 and η11 = η22 = η33 = −1. ∇μ designates the partial derivative with respect to the space-time coordinate xμ. The notation ∇ designates the three-dimensional nabla operator. We use the dummy index rule. Special-relativistic MHD equations associate fluid equations with Maxwell's equations, in which the displacement current and Poisson's equation should be retained. The fluid equations consist of a conservation equation for particle number, valid in the absence of reactions among particle species, and of the four components of the energy and momentum conservation equations. The law of conservation of particle number is written as: (12)The density nF is the proper spatial number density of particles, that is, their density measured in the instantaneous rest frame of the fluid. The four components uμ are those of the dimensionless four-velocity of the fluid in the considered rest frame: (13)The Lorentz factor γ refers here to the bulk fluid motion. The number density in the observer's frame is the fourth component of the density-flux four-vector, nFγ. The equations of conservation of energy and momentum of matter are lumped in the four-tensorial equation: (14)The 's are the components of the energy-momentum tensor of matter and the components are those of the electromagnetic force density four-vector. By using Maxwell's equations, this four-vector can be written in conservative form and Eq. (14) can be given the form: (15)The 's are the components of the electromagnetic energy-momentum tensor. They can be expressed in terms of the electromagnetic field strength tensor F or in terms of the electric and magnetic fields observed in the chosen reference frame. Its time-time component is the electromagnetic energy density, its space-time components are the three components of the Poynting vector divided by c and its space-space components form a second-rank tensor of the three-dimensional Euclidean space, the Maxwell stress tensor: (16)The symbol δ represents the second rank unit tensor. The matter energy-momentum tensor of a cold pressureless fluid can be written in the absence of non-ideal effects such as viscosity as (17)Without internal heat, the number conservation Eq. (12) reduces to a conservation equation for proper mass, because in this case ρF = m nF, m being the rest mass of particles. Equation (12) can then be written in three-dimensional notations as (18)Here, we need not solve the energy conservation equation because the medium is regarded as cold. We only consider the spatial components of the equivalent Eqs. (14) or (15). From Eq. (14) we obtain, denoting the charge and current density by ρe and j respectively: (19)From Eq. (15) we obtain the equivalent equation: (20)The components of the Maxwell stress tensor may be transformed to account for the perfect MHD relation (21)The components of the electric field and those of the Maxwell stress tensor are easily calculated in a frame where the x-axis is taken to be along the direction of the fluid velocity v. Some algebra then yields the following expression, where the indices t (transverse) and l (longitudinal) refer to a component of a vector perpendicular or parallel to the velocity v of the fluid: (22)The magnetic field evolution equation, deduced from Faraday's equation and the perfect MHD relation, writes (23)The non-relativistic theory of Neubauer (1980) only considers the Alfvénic wake of the satellite. Indeed, fast MHD disturbances propagate isotropically in the low-βP limit and decrease in amplitude with distance from the source (βP is the ratio of the plasma pressure to the magnetic pressure). These disturbances do not create any concentrated current system. The slow mode propagates in a low-βP plasma much slower than Alfénic perturbations and the associated disturbances, though channelled by the magnetic field, soon become spatially separated from the Alfénic wake. Actually, slow-mode perturbations barely propagate at all in a cold pulsar wind and carry negligible current. The effects of compressive perturbations in the non-relativistic situation have been discussed by Wright & Schwartz (1990), who have shown that compressive plasma wave modes, though necessarily excited, contribute one order of magnitude less to the current flow and to the energy budget than shear Alfvén perturbations do. We therefore follow Neubauer in concentrating on purely Alfvénic motions. We assume that the fluid motions triggered when the planet passes by are sub-relativistic in the rest frame RW of the unperturbed wind and that the changes of the formal Alfvén velocity are similarly sub-relativistic. We do not assume, however, that the formal Alfvén speed calculated from the total field, B′/(μ0ρ′)1/2, is less than the speed of light. Our assumption of non-relativistic Alfvénic motions in RW implies that div v′ = 0. It does not follow, however, that the same relation also holds true in the observer's frame RO because the wind flow is relativistic in this frame. In RW, the electric terms of the Maxwell stress tensor are of the order of v′2/c2 less than the magnetic terms and can be neglected. Accounting for the relation div v′ = 0, Eq. (23) can be written as (24)Considering Eqs. (21) and (22), the equation of motion (20) becomes, in RW, (25)
4. An Alfvénic first integral
The computation of the non relativistic Alfvén wing given by Neubauer (1980) is based upon the fact that in simple non-linear Alfvénic wave motions, the velocity Vs = v − s cA is a first integral. In this relation, v is the fluid's velocity, cA the vectorial Alfvén velocity associated with the perturbed field, and the sign s = ± 1 depends on the sense of propagation of the perturbation. This relation can be transposed in a differential form as dB = kdv, where k = (μ0ρ)1/2. Moreover, the modulus of the magnetic field is a time invariant and, because of the uniform boundary conditions B = B0, this modulus is constant over the whole space.
As Neubauer, we look for a solution where dB′ = kdv′ and where B′ is constant. Then, setting b′ = B′/B′ and (26)we can write Eqs. (24) and (25) in the form where . The two first terms of Eq. (27) are analogous to those of classical MHD, when VA ≪ c. The two others are specific to fast variations of the electric field, when the displacement current is taken into account. We solve this system in the following way: we first ignore the last two terms of Eq. (27) and solve the resulting system (27) − (28), which can then be written as We then check whether the last two terms in Eq. (27) vanish or are negligible. These terms are (31)Considering Eqs. (29) and (30), the proportionality of dB′ and dv′ is obtained for k = sλ, and these two equations become equivalent to Equation (32) has a first integral , (34)In the region not perturbed by the planet, v′ = 0, and . Therefore, In order of magnitude, λ ~ B′/c, and the approximation v′ ≪ c implies that . Therefore, this is equivalent to an hypothesis of linear perturbation. This remark also holds for the computations of Neubauer (1980). At this stage, it is necessary to evaluate the terms in Eq. (31). Using the above relations, these terms are (38)where is the direction of the unperturbed magnetic field in the wind's frame of reference. The quantity in Eq. (38) does not vanish but it is negligible as long as v′ ≪ c in comparison to the terms in Eq. (29), which are of the order of (B′2/c)db′/dt′. Therefore, in the linear approximation, the solution given by Eqs. (32 − 37) is correct.
The first integral of Eq. (34) must now be computed in the observer's frame of reference RO. It will be used in the next section to derive the value of the electric current associated to the Alfvén wings.Let us write the velocity and the magnetic field as the sum of a longitudinal component, parallel to v0, and a transverse vector component. The transforms of the velocity and of the magnetic field are where γ0 is the Lorentz factor of the unperturbed wind. For the transform of the magnetic field, Eq. (21) has been taken into account. Equation (34) becomes (44)For a first order development, we note the velocity perturbation and the magnetic perturbation, (45)To the first order, Eq. (44) becomes (46)which can be rewritten Considering the purely geometric relation (47)we have (48)Because this vector is constant, its longitudinal and transverse parts relatively to the constant vector v0 are also two distinct constant entities. We can recombine the longitudinal and transverse components in the following way Then we can define a new first integral vector, (49)where the constant number α is defined by (50)In spite of a greater complexity, this vector presents some analogy with the first integral found in the non-relativistic case by Neubauer (written in the first lines of the present section). This will be used in the next section to derive the current flowing along the Alfvén wing, in a similar way to those developed in Neubauer (1980). The parameter λ, given in Eq. (26), can be expressed as a function of the unperturbed wind parameters, (51)Because ∇·v′ = 0, the density ρ′ is invariant along any line of flow; that is why we noted it instead. We set These are mixtures of the magnetic field in the frame RO of the observer and of the density in the proper frame RW of the wind in terms of which the factor λ can be written as (55)
5. Current carried by an Alfvén wing
Neubauer (1980) has shown that the electric current density carried by an Alfvén wing is related to the divergence of the electric field through the relation μ0 j·Vs = Σ div E, where the conductance , cA being the classical Alfvén velocity, and MA = v0/cA. In this section, we derive an analogous relation for the relativistic plasma flow, keeping our previous assumptions. From the perfect MHD relation (21) we calculate div E in the observer's frame RO: (56)To the first order, (57)From Eq. (49), the curl of the velocity is where (60)Including Eqs. (58) in (57), we find (61)For further convenience, we note (62)In RO, the Alfvén wave is stationary, therefore the partial time derivatives are null, and Ampère's equation is simply (63)Then, from Eq. (61), (64)Let Js be the projection of the current density along the direction of the constant vector Us of Eq. (49). Equation (64) can be written as (65)Let θ = π/2 − (B0,v0) be the complement of the angle made in RO by the ambient magnetic field and the flow velocity. The modulus of Us (Eq. (49)) is (66)and then When cA ≪ c, we are in the conditions studied by Neubauer, and we find the same result as in his paper (given in the beginning of this section). If γ0 ≫ 1 and cA ≫ c, that is relevant for a pulsar's wind, XA ≫ 1 and (70)a conductance that is associated with the impedance of vacuum, equal to ℛ∞ ≡ μ0c = 377 Ohm. The two directions of the current flows correspond to the invariant vectors U + and U − . The geometrical configuration of this solution is shown in Fig. 2.
Fig. 2
Alfvénic wake of the planet seen from above the equatorial plane.
|Open with DEXTER
Now, we can quite directly adapt the conclusions of Neubauer (1980) to the relativistic inductor. This author considers a specific model of the wake-aligned currents in the Alfvén wing, which he assumes to be flowing on the surface of an infinite cylinder tangent to the planet's surface, with its axis parallel to Alfvénic characteristics. Equation (67) implies that for these currents the divergence of the electric field vanishes except on the cylinder's surface. The electric potential can then be found by solving Laplace's equation, assuming the electric field inside the cylinder to be constant, of intensity Ei. This simple assumption is motivated by the difficulty to solve for the electromagnetic and flow structure in the immediate vicinity of the solid body. The free parameter Ei is the electric field along the planet caused by its ionosphere or surface internal resistance. At large distances from the wake, the electric field converges to the convection field E0 given by the perfect MHD relation (21) in the unperturbed wind. Once the electric potential is found, the magnetic field and current distribution in the wake can be deduced, using in particular Eq. (67).
Neubauer gives useful expressions for the total current I flowing along an Alfvén wing and for the Joule dissipation power in the solid body, ĖJ. Writing RP for the planet's radius, he obtains \arraycolsep1.75ptThe Joule dissipation is maximum when Ei = E0/2. In our estimations, we shall use Neubauer's values for I and ĖJ. Up to unimportant numerical factors, the results (71) − (72) are simply obtained by considering the current I to be driven in a resistive load of resistance by a generator of electromotive force U0 = 2E0RP applied on two opposite sides of a planet of internal resistance ℛP. Neubauer's parameter Ei is related to ℛP by (73)It is very difficult to know precisely the value of ℛP. We therefore regard it, or Ei, as unspecified parameters. The planet's electrical resistance depends on its constitution, on the path of electric currents in it, and on the existence or absence of some form of ionosphere. The conductivity of terrestrial silicate rock is of the order of σrock = 10-3 Mho m-1 (Cook 1973). Assuming that the wake current closes through a layer of thickness h at the surface of the planet, the electrical resistance ℛP of the latter would be of the order of , which numerically amounts to ℛP ~ (hkm)-1. As soon as h exceeded a few meters, which for this low conductivity is reached in a very short time, ℛP would be comparable to or less than ℛ∞, even though the rock intrinsically is a poor conductor. A second-generation planet, which could be partly metallic or a partly molten body, could have lower resistances.
6. Discussion and conclusion
We showed that a planet orbiting a pulsar develops a system of Alfvén wings caused by its interaction with the sub-Alfvénic Poynting-flux-dominated pulsar wind. A system of strong electric currents is set. Although this current cannot reach the inner pulsar's magnetosphere, it is nevertheless interesting to compare it to the current at the origin of the pulsar's magnetospheric activity, the Goldreich-Julian current JGJ. This latter current results from the electromotive field generated by the fast rotation of the highly magnetized neutron star and its surrounding magnetosphere. For a dipole magnetic field, the Goldreich-Julian current density is (74)and the total current is of the order of (75)where is the polar cap radius (Kirk et al. 2009). Various values of the Goldreich-Julian current IGJ are given in Table 1. A look at Table 3 allows for comparisons between IAW and IGJ. Obviously, for the four known planets the electric current in the Alfvén wings is lower than the Goldreich-Julian current by three orders of magnitude. It is also much lower for small bodies. But a planet orbiting a "standard" pulsar with a typical 1 second period and 1012 G magnetic field would have an Alfvén wing current IAW of similar amplitude as the Goldreich-Julian current IGJ. This is not negligible when we see that IGJ is the basic engine of the pulsar's electrodynamics.
The practical consequences of such a current are expected to be of two kinds: we show in a companion paper (Mottez & Heyvaerts 2011) that it can exert an ortho-radial force upon the planet that can, if the magnetic to mechanical energy coupling is efficient enough, have an incidence on the orbit of small circum-pulsar objects such as asteroids or comets. The second incidence, more relevant to massive objects such as planets, is a possibly associated electromagnetic signature, which might be detectable.
Does the Alfvén wing dominate in terms of energy, the direct mechanical action exerted by the wind on the companion? To answer this question, we can compare the flux of magnetic energy, FM with the flux of mechanical energy, FK, received the companion by direct impingement. The ratio of the Poynting flux to the mechanical energy flux is (76)Introducing σ0 and Ψ with the Eqs. ((5), (6), (10)), and v0r ~ c, (77)In the case discussed above, where , and σ0 ≫ 1, (78)Therefore, we expect that for a Poynting-flux-dominated wind most of the energy exchange with the pulsar's companion comes from the magnetic field. Equation (72) provides a more precise insight of what is effectively involved in the wind-companion interaction. Considering Ei = E0 and E0 ~ cBφ, (79)This amounts to the totality of the Poynting flux intercepted by the pulsar's companion. It is therefore higher (by a factor ) than the mechanical energy captured by direct impigement.
We assume that the wind velocity v0 is slower than the Alfvén wave velocity VA. Otherwise, there would be no Alfvén wing. For an ideal MHD radial wind, the Lorentz factor asymptotically approaches and Eq. (9) shows that the wind remains sub-Alfvénic at any distance. If, however, it is formally considered that the asymptotic Lorentz factor γ0∞ scales as σa instead, with an exponent a ≠ 1/3, then if a > 1/3, MA∞ = 1 + σa − 1 − σ − 2a ~ 1 + σa − 1 > 1. Therefore, in that case, a transition from a sub-Alfvénic to a super-Alfvénic wind occurs at a finite distance. Observations of the equatorial sectors of winds driving pulsar wind nebulae show lower values of the asymptotic magnetization (Kennel & Coroniti 1984a,b; Gaensler et al. 2002), and various authors suggest that the asymptotic value of the Lorentz factor is rather γ∞ ~ σ0. Arons (2004) argues that dissipation must occur in the asymptotic wind zone to understand the observed high Lorentz factors and the low magnetization. Begelman & Li (1994) show that when the flux tubes diverge faster than radially, the fast magnetosonic point can occur closer to the light cylinder, implying an even closer Alfvénic point. Then, the existence of Alfvén wings would depend on the distance from the star to the planet, combined with the effect of a non-radial diverging wind flow, or dissipation.
Let us return to the hypothesis of a planet in a sub-Alfvénic wind. The present work provides only orders of magnitude estimates for the emitted current. The behaviour of the Alfvén wing at close vicinity of the planet would need a more detailed study. We considered here, as in many other papers concerning pulsars, the case of a neutron star magnetic field that is aligned with the rotation axis. The study of oblique rotators raises more complicated problems. The pulsar wind may have different properties and carry even in the equatorial plane a non-zero Bθ component that oscillates at the pulsar rotation rate Ω∗. An Alfvén wavelength (propagating at ~ c) with P = 6 ms (case of PSR B1257+12) is of the order of 1800 km, which is less than a typical planetary radius. This would question the assumption of stationarity, though less severely for a standard pulsar with P ~ 1s, where the wavelength (about 300 000 km) would be much larger than the planetary radius.
In spite of the preliminary character of our model, our study shows that the consideration of Alfvén wings associated to planets that orbit pulsars deserve some attention.
The question of the radio emissions that are possibly associated to the Alfvén wings will be addressed in a
forthcoming paper. These emissions would provide astronomers with observational data relevant to the wind/planet interaction.
This paper was inspired by discussions with Silvano Bonazzola (LUTH, Obs. Paris-Meudon). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and The Extrasolar Planets Encyclopaedia (http://exoplanet.eu/index.php), maintained by Jean Schneider at the LUTH, and the SIO, at the Observatoire de Paris, France.
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All Tables
Input data of the pulsars.
Input data concerning the planets: mass, radius, orbital period, semi-major axis, excentricity.
Electric potential drop and total electric current associated to the Alfvén wing.
All Figures
Fig. 1
Schematic view of a unipolar inductor.
|Open with DEXTER
|In the text
Fig. 2
Alfvénic wake of the planet seen from above the equatorial plane.
|Open with DEXTER
|In the text
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Wednesday's programme will feature panelists Dr. Rondalyn Dennis-Bradshaw, Dean of the Division of Health Sciences at CFBC and Ms. Michelle Crawford, graduate of the CFBC BScN Nursing Programme.
The two are expected to give an in-depth look at the programmes being offered at the tertiary institution, as well as the requirements needed for one to pursue studies and a career in this important field.
"Working for You" offers news, views, reviews, interviews and all the happenings of the Team Unity Administration, which has pledged transparency, accountability, good governance and a fair share for all citizens of the Federation.
The programme features government officials, heads of government departments, permanent secretaries and other government officials who will provide you with timely, relevant and accurate information as it relates to the social, economic, human, political and sustainable development of St. Kitts and Nevis
"Working for You" is carried live every Wednesday on ZIZ, WinnFM and Sugar City Rock from 1:30-3:00pm and rebroadcast on Freedom FM, Von Radio on Thursdays from 7:30-9:00am and 10:30-12:00pmrespectively, and CBN-Radio on Sundays from 5:00-6:30pm. The programme is also streamed live on the SKNIS Facebook page: https://www.facebook.com/sknismedia/


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People who read, raise your hands. 🙂 Hi everyone, it is the last day of our weekday and we are gearing towards the weekend! Hooray!
Reading is an activity that is very close to my heart. It literally brings me to a place where I could just be immersed in an alternative reality. To put into perspective, I spend around 20 minutes in a clothing store but could easily spend 2 hours in a bookstore. That's how much I love being surrounded by books. In a world where everything is getting extremely busy, it could be challenging to sit down and actually read something. However, there is nothing more rewarding than keeping our minds agile. I am a big advocate for people to pick up reading. I believe knowledge empowers you. It doesn't matter what type of books you read (I mean books not tabloid magazines), you will keep firing those neurones in your brain to keep it active. A active mind leads to a better overall wellbeing. Thus, #pickabookFriday is where I will talk briefly about a book I've read in the hope that it would inspire everyone to take up this meaningful activity. 🙂
In this first post of this series, I chose The Little Prince. It is my favourite book mainly because of the strong messages embedded in it which I could relate to at any stage of my life. This lovely book is packed with beautiful metaphors and analogy. It discusses the different roles people assume in life, the varying characters of humans, different perspective in looking at life issues and most importantly friendship and love. No matter what stage of life you are at, you will definitely take away a meaningful message. The beauty of this book lies in its ability to ignite inner reflection on what is important for you. I believe it is a book that will appeal to anyone.
There are many insightful moments in the book but one quote stood out from the rest:
"One sees clearly only with the heart. Anything essential is invisible to the eyes"
What are the most beautiful things for you?
Happy reading everyone and have a great weekend!
xx, Mielyn


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Berlin pops up in bid to capture start-ups from Canary Wharf and Old St
PUBLISHED: 14:24 11 October 2015 | UPDATED: 14:24 11 October 2015
The Germans have popped up in London's East End to entice new high-tech enterprises under the nose of Canary Wharf and Old Street Tech City.
They occupied two vacant shops in Bethnal Green at the weekend aiming to persuade budding entrepreneurs to relocate to Berlin.
The 'Berlin Partner for Business & Technology' has begun a marketing campaign with 'Visit Berlin' launched with pop-up stores in five European cities including London to market Berlin as "a creative, innovative and liveable metropolis" for new businesses.
The pop-up stores are open for a week to showcase Berlin in design, fashion, furniture, food, life-style and technology.
The pop-up stores are open for a week to showcase Berlin in design, fashion, furniture, food, life-style and technology.
They are hoping to offer "an alternative" to Old Street's Tech City, while Lufthansa has its Telekom "innovation hub" in Berlin rivalling Canary Wharf's Level39 start-up accelerator.
Start-ups in the German federal capital accumulated more venture cash than young entrepreneurs from London in 2014 for the first time ever, it is claimed. The trend is said to have continued in the first half of this year, with start ups attracting 1.4 billion euros compared to 1.1 billion in London.
If you value what this story gives you, please consider supporting the East London Advertiser. Click the link in the orange box below for details.


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Hymn Lyrics Search - Name That Hymn
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by herringdan8858 » Mon Jun 25, 2018 7:31 am
lhylton wrote: ↑Wed Sep 03, 2008 7:59 am
He never left me, though I turned my back on Him
Living in a world of sin, trying to run away again.
He never left me, when I chose to walk away.
Even when I couldn't pray, He never left me.
So many directions, the roads look the same
He gave me instructions, I disregarded in shame
Then sudden destruction soon came my way.
I'll have to say, I've got me to blame.
I chose a wrong road cause it looked good to me
I walked blindly onward, I just could not see
I was lost and I was dying, but now I am trying
I reached out to Jesus, you know He reached out to me.
Thanks for asking ... I wrote the song.
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text:
Friday, March 31, 2006
Creekistan, We Have Puppy
Well, actually, not quite yet. Next week we will be the proud "parents" of a rescued puppy named Bandit. His mother was killed by a car when he and his litter-mates were 1 week old. As far as I can tell, he is the only surviving puppy left. But he's doing great! We met him today at the shelter.
We've got some things to take care of before we can bring him home, but everyone, including my husband, is excited.
Wish us luck!


text:
Everything that hadn't been said about the election already but should have been said long ago is at Pittsblog 2.0.
Diana Nelson Jones' City Walkabout is getting interesting. For one thing she is getting up on her soapbox — for another, she has leapt ahead of the curve on issues related to the Mayor's aggressive demolitions policy.
Happy urban-dwelling Democrats: are we going to make a big deal about the Marriage Equality Bill? I say, we might as well! Who's first? Pgh Lesbian Correspondents; OneFiveTwoOneOne; Peaks and Gutters.
Political campaign operative -slash- Democratic committeeman -slash- government whistle blower -slash- community organizer -slash- investigative blogger Matt Hogue writes:
Here is what I have to say about Wagner. What exactly has he done for his neighborhood of Beechview? NOTHING. Why does this man seem to exert so much power and influence? It's all about that Ward Chairmanship that he is barely hanging onto. Why is this guy still in power? Intimidation? Luck? I think it's a little bit of both. All throughout the campaign I met numerous Democratic Committee members who were deathly afraid of not putting a Patrick Reilly sign up in their yard for fear of Wagner coming knocking at their doors. What a disgraceful way to rule your Committee. (Pgh Hoagie)
Here's what I have to say about that.
1) It pleases me that chaos and ill-will are still festering in the Committee.
2) It's distinctly possible that I have no idea what I'm talking about, but … nothing Matt H writes here seems particularly troubling. Unless he would like to define "shenanigans," which is a word I once tried to get Rich Lord to print to no avail seeing as how it is vague and subtly evasive. Everything I know about the Wagner operation stems from reading the HUDDLER, which I think we have established already is some form of surreal glimpse into the Wagnerian mind. And those people seem just fine.
3) However, Hogue does go on to call for Pete Wagner's resignation from the Committee for "strong-arming", "threats", and "goon"-ish behavior, so for some in our audience that might be newsworthy and important.
We close with Hall & Oates. Have a nice weekend.


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Can we please have a document crated that has a comprehensive list of tools that require a Customer Success Manager to activate?
In most cases, this is indicated in the documentation of the tool you're reviewing, but this isn't always the case, for example the administration documents for Attendance:
The document should also explain why each tool is not an administrator option, and identify any additional processes required to activate the tool in question.
Several examples include:
Attendance (Roll Call)
Canvas Commons
Office 360 (for international schools)
Recurring calendar events
And many more …