<commit_before>{
	"stages": ["Main Sequence","Main Sequence","Red Giant","Red Giant","Red Giant","Red Giant","Red Giant","Blue Giant","Blue Giant","Blue Giant","White Dwarf","White Dwarf","White Dwarf","Neutron Star","Black Hole","Obliteration"],
	"phrasebook": {
		"modes": { "normal": "Normal","advanced": "Advanced", "toggle": "Toggle mode" },
		"about": { "title": "About", "content" : "<p>Star in a Box allows you to explore one of the most enigmatic tools in astronomy - the <a href=\"http://lcogt.net/book/h-r-diagram\">Hertzsprung-Russell diagram</a>.</p><p>When you first open the box you start with a star with the same mass as the Sun but you can change this to a different mass at any time. The tracks that you see on the graph (on the left) map the lifecycle of the star. You can play the animation of the star moving around the diagram, and see how its brightness, size, surface temperature, and mass change in the panels on the right.</p><p>Stars can take billions of years to go through their lives with the dramatic events taking place in relatively short periods of time. In the animation we speed up time when the star is not really changing much and slow things down for the dramatic phases of the star's life.</p><h3>Keyboard controls:</h3>%CONTROLLIST%<h3>Acknowledgments</h3><p><b>Design &amp; Development</b>: <a href=\"http://jyardley.co.uk\"><NAME></a>, <a href=\"http://www.strudel.org.uk/\"><NAME></a>, <a href=\"http://lcogt.net/user/egomez\"><NAME></a>, <a href=\"http://www.astro.cf.ac.uk/contactsandpeople/?page=full&id=151\"><NAME></a> &amp; <NAME></p><p>Supported by <a href=\"http://www.stfc.ac.uk/\">STFC</a>, <a href=\"http://lcogt.net/\">LCOGT</a> &amp; <a href=\"http://www.cf.ac.uk/\">Cardiff University</a></p>" },
		"data": { "title": "Data Table", "content": "This is a summary of the star that is currently selected. Mass: <strong>%MASS%</strong>.</p>%TABLE%<p>Download data as %CSV%.</p>" },
		"keys": {
			"play" : "Play",
			"lid" : "Open lid",
			"mode" : "Toggle mode",
			"size" : "Size panel",
			"temperature" : "Temperature panel",
			"luminosity" : "Brightness panel",
			"stage" : "Stage panel",
			"mass" : "Mass panel"
		},
		"intro": {
			"title": "Welcome!",
			"content": "<p>You are now the proud owner of Star In A Box.</p><p>Inside this box you can animate the different stages in a star's life and see how its brightness, size, and mass change with time.</p><p>Once you've opened the box just <strong>click the play button</strong> to start animating.</p>"
		},
		"open": "&lsaquo; Open the lid",
		"close": "Close the lid &rsaquo;",
		"preparing": "Your star is being prepared.<br />Please wait...",
		"sun": "Sun",
		"stage": "Stage",
		"radius": "Radius",
		"radiusunit": "compared to the Sun",
		"duration": "Duration",
		"timescale": "million years",
		"longtime": "A very long time",
		"lum": "Brightness",
		"lumunit": "compared to the Sun",
		"temp": "Temperature",
		"tempunit": "Kelvin",
		"cooldown": "Cool down from %TEMP%",
		"cooling": "Cooling",
		"mass": "Mass",
		"massunit": "&times; Sun",
		"ms": "Main Sequence",
		"speeds": ["fastest","fast","normal","slow","slowest"],
		"buttons": {
			"play": "Start/pause",
			"reset": "Back to the start of your star's life",
			"size": "Compare the size",
			"temperature": "Surface temperature",
			"luminosity": "Brightness",
			"stage": "Stages in your star's life",
			"mass": "Mass"
		},
		"help": {
			"tab": "Information",
			"content": {
				"m0.2" : "<h1> 0.2 Time The Mass of The Sun </h1><h3>Main Sequence</h3><p>Stars around or less than half the mass of the Sun start off as low mass Main Sequence stars. Here, they are in very stable states where they fuse hydrogen atoms into helium as a source of energy.</p><img src='http://www.spaceanswers.com/wp-content/uploads/2013/01/Red-dwarf-main-image.jpg'/><h3>Red Giant </h3><p>When the core of the star runs out of hydrogen to fuse into helium, the outer layers of the star begin to swell and the surface temperature of the star cools, the star also changes appearance to become redder. Since stars of this mass are too small to initiate helium fusing in the core, the star burns out all of its hydrogen supply, leaving the helium core behind, as what is known as a 'Helium White Dwarf'.</p><img src='http://www.dailygalaxy.com/.a/6a00d8341bf7f753ef017ee8bb15b8970d-500wi'/>",
				"m0.65" : "<h1> 0.65 Time The Mass of The Sun </h1><h3>Main Sequence</h3><p>Stars around or less than half the mass of the Sun start off as low mass Main Sequence stars. Here, they are in very stable states where they fuse hydrogen atoms into helium as a source of energy.</p><img src='http://www.spaceanswers.com/wp-content/uploads/2013/01/Red-dwarf-main-image.jpg'/><h3>Red Giant </h3><p>When the core of the star runs out of hydrogen to fuse into helium, the outer layers of the star begin to swell and the surface temperature of the star cools, the star also changes appearance to become redder. Since stars of this mass are too small to initiate helium fusing in the core, the star burns out all of its hydrogen supply, leaving the helium core behind, as what is known as a 'Helium White Dwarf'.</p><img src='http://www.dailygalaxy.com/.a/6a00d8341bf7f753ef017ee8bb15b8970d-500wi'/>",
				"m1" : "<h1> Stars With The Mass of The Sun </h1><h3>Main Sequence</h3><p>The main sequence stage is the longest inhabited stage by a star. Here the star remains stable for millions to billions of years, fusing hydrogen atoms into helium atoms as fuel.</p><h3>Red Giant</h3><img src='http://earthsky.org/brightest-stars/antares-rivals-mars-as-the-scorpions-heart'/><p>When all of the hydrogen in the core turns into helium, the outer layers of the star begin to swell and become redder as they do in stars of around 0.2-0.65 times the mass of the Sun. However, for stars the same mass as the Sun and up to 8 times the mass of the Sun, the core becomes hot enough to fuse helium into heavier elements such as carbon and oxygen. However they still aren't heavy enough to fuse carbon and oxygen into heavier elements in the core. Eventually the hydrogen and helium layers of the star fade away leaving a 'Carbon/Oxygen White Dwarf' similar to low mass stars.</p><img src='http://www.dailygalaxy.com/.a/6a00d8341bf7f753ef017ee8bb15b8970d-500wi'/>",
				"m2" : "<h1> 2 Time The Mass of The Sun </h1><h3>Main Sequence</h3><p>The main sequence stage is the longest inhabited stage by a star. Here the star remains stable for millions to billions of years, fusing hydrogen atoms into helium atoms as fuel.</p><h3>Red Giant</h3><img src='http://earthsky.org/brightest-stars/antares-rivals-mars-as-the-scorpions-heart'/><p>When all of the hydrogen in the core turns into helium, the outer layers of the star begin to swell and become redder as they do in stars of around 0.2-0.65 times the mass of the Sun. However, for stars the same mass as the Sun and up to 8 times the mass of the Sun, the core becomes hot enough to fuse helium into heavier elements such as carbon and oxygen. However they still aren't heavy enough to fuse carbon and oxygen into heavier elements in the core. Eventually the hydrogen and helium layers of the star fade away leaving a 'Carbon/Oxygen White Dwarf' similar to low mass stars.</p><img src='http://www.dailygalaxy.com/.a/6a00d8341bf7f753ef017ee8bb15b8970d-500wi'/>",<commit_msg>tweaked en.json for 1Solar Mass star<commit_after>{
	"stages": ["Main Sequence","Main Sequence","Red Giant","Red Giant","Red Giant","Red Giant","Red Giant","Blue Giant","Blue Giant","Blue Giant","White Dwarf","White Dwarf","White Dwarf","Neutron Star","Black Hole","Obliteration"],
	"phrasebook": {
		"modes": { "normal": "Normal","advanced": "Advanced", "toggle": "Toggle mode" },
		"about": { "title": "About", "content" : "<p>Star in a Box allows you to explore one of the most enigmatic tools in astronomy - the <a href=\"http://lcogt.net/book/h-r-diagram\">Hertzsprung-Russell diagram</a>.</p><p>When you first open the box you start with a star with the same mass as the Sun but you can change this to a different mass at any time. The tracks that you see on the graph (on the left) map the lifecycle of the star. You can play the animation of the star moving around the diagram, and see how its brightness, size, surface temperature, and mass change in the panels on the right.</p><p>Stars can take billions of years to go through their lives with the dramatic events taking place in relatively short periods of time. In the animation we speed up time when the star is not really changing much and slow things down for the dramatic phases of the star's life.</p><h3>Keyboard controls:</h3>%CONTROLLIST%<h3>Acknowledgments</h3><p><b>Design &amp; Development</b>: <a href=\"http://jyardley.co.uk\"><NAME></a>, <a href=\"http://www.strudel.org.uk/\"><NAME></a>, <a href=\"http://lcogt.net/user/egomez\"><NAME></a>, <a href=\"http://www.astro.cf.ac.uk/contactsandpeople/?page=full&id=151\"><NAME></a> &amp; <NAME></p><p>Supported by <a href=\"http://www.stfc.ac.uk/\">STFC</a>, <a href=\"http://lcogt.net/\">LCOGT</a> &amp; <a href=\"http://www.cf.ac.uk/\">Cardiff University</a></p>" },
		"data": { "title": "Data Table", "content": "This is a summary of the star that is currently selected. Mass: <strong>%MASS%</strong>.</p>%TABLE%<p>Download data as %CSV%.</p>" },
		"keys": {
			"play" : "Play",
			"lid" : "Open lid",
			"mode" : "Toggle mode",
			"size" : "Size panel",
			"temperature" : "Temperature panel",
			"luminosity" : "Brightness panel",
			"stage" : "Stage panel",
			"mass" : "Mass panel"
		},
		"intro": {
			"title": "Welcome!",
			"content": "<p>You are now the proud owner of Star In A Box.</p><p>Inside this box you can animate the different stages in a star's life and see how its brightness, size, and mass change with time.</p><p>Once you've opened the box just <strong>click the play button</strong> to start animating.</p>"
		},
		"open": "&lsaquo; Open the lid",
		"close": "Close the lid &rsaquo;",
		"preparing": "Your star is being prepared.<br />Please wait...",
		"sun": "Sun",
		"stage": "Stage",
		"radius": "Radius",
		"radiusunit": "compared to the Sun",
		"duration": "Duration",
		"timescale": "million years",
		"longtime": "A very long time",
		"lum": "Brightness",
		"lumunit": "compared to the Sun",
		"temp": "Temperature",
		"tempunit": "Kelvin",
		"cooldown": "Cool down from %TEMP%",
		"cooling": "Cooling",
		"mass": "Mass",
		"massunit": "&times; Sun",
		"ms": "Main Sequence",
		"speeds": ["fastest","fast","normal","slow","slowest"],
		"buttons": {
			"play": "Start/pause",
			"reset": "Back to the start of your star's life",
			"size": "Compare the size",
			"temperature": "Surface temperature",
			"luminosity": "Brightness",
			"stage": "Stages in your star's life",
			"mass": "Mass"
		},
		"help": {
			"tab": "Information",
			"content": {
				"m0.2" : "<h1> 0.2 Time The Mass of The Sun </h1><h3>Main Sequence</h3><p>Stars around or less than half the mass of the Sun start off as low mass Main Sequence stars. Here, they are in very stable states where they fuse hydrogen atoms into helium as a source of energy.</p><img src='http://www.spaceanswers.com/wp-content/uploads/2013/01/Red-dwarf-main-image.jpg'/><h3>Red Giant </h3><p>When the core of the star runs out of hydrogen to fuse into helium, the outer layers of the star begin to swell and the surface temperature of the star cools, the star also changes appearance to become redder. Since stars of this mass are too small to initiate helium fusing in the core, the star burns out all of its hydrogen supply, leaving the helium core behind, as what is known as a 'Helium White Dwarf'.</p><img src='http://www.dailygalaxy.com/.a/6a00d8341bf7f753ef017ee8bb15b8970d-500wi'/>",
				"m0.65" : "<h1> 0.65 Time The Mass of The Sun </h1><h3>Main Sequence</h3><p>Stars around or less than half the mass of the Sun start off as low mass Main Sequence stars. Here, they are in very stable states where they fuse hydrogen atoms into helium as a source of energy.</p><img src='http://www.spaceanswers.com/wp-content/uploads/2013/01/Red-dwarf-main-image.jpg'/><h3>Red Giant </h3><p>When the core of the star runs out of hydrogen to fuse into helium, the outer layers of the star begin to swell and the surface temperature of the star cools, the star also changes appearance to become redder. Since stars of this mass are too small to initiate helium fusing in the core, the star burns out all of its hydrogen supply, leaving the helium core behind, as what is known as a 'Helium White Dwarf'.</p><img src='http://www.dailygalaxy.com/.a/6a00d8341bf7f753ef017ee8bb15b8970d-500wi'/>",
				"m1" : "<h1> Stars With The Mass of The Sun </h1><h3>Main Sequence</h3><p>The main sequence stage is the longest inhabited stage by a star. Here the star remains stable for millions to billions of years, fusing hydrogen atoms into helium atoms as fuel.</p><h3>Red Giant</h3><div style='width:100%'><div style='float:left;width:200px'><img src='config/images/RedGiant.jpeg' style='width:95%'/></div><p>When all of the hydrogen in the core turns into helium, the outer layers of the star begin to swell and become redder as they do in stars of around 0.2-0.65 times the mass of the Sun. However, for stars the same mass as the Sun and up to 8 times the mass of the Sun, the core becomes hot enough to fuse helium into heavier elements such as carbon and oxygen. However they still aren't heavy enough to fuse carbon and oxygen into heavier elements in the core.</p></div><div style='clear:both'></div><h3>White Dwarf</h3><div style='width:100%'><div style='float:left;width:200px'> <img src='http://www.dailygalaxy.com/.a/6a00d8341bf7f753ef017ee8bb15b8970d-500wi' style='width:95%'/></div>Eventually the hydrogen and helium layers of the star fade away leaving a 'White Dwarf' similar to low mass stars.</p></div>",
				"m2" : "<h1> 2 Time The Mass of The Sun </h1><h3>Main Sequence</h3><p>The main sequence stage is the longest inhabited stage by a star. Here the star remains stable for millions to billions of years, fusing hydrogen atoms into helium atoms as fuel.</p><h3>Red Giant</h3><img src='http://earthsky.org/brightest-stars/antares-rivals-mars-as-the-scorpions-heart'/><p>When all of the hydrogen in the core turns into helium, the outer layers of the star begin to swell and become redder as they do in stars of around 0.2-0.65 times the mass of the Sun. However, for stars the same mass as the Sun and up to 8 times the mass of the Sun, the core becomes hot enough to fuse helium into heavier elements such as carbon and oxygen. However they still aren't heavy enough to fuse carbon and oxygen into heavier elements in the core. Eventually the hydrogen and helium layers of the star fade away leaving a 'Carbon/Oxygen White Dwarf' similar to low mass stars.</p><img src='http://www.dailygalaxy.com/.a/6a00d8341bf7f753ef017ee8bb15b8970d-500wi'/>",
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