Oxygen-rich droplets and the enrichment of the ISM
Oxygen-rich droplets and the enrichment of
the ISM
Grażyna Stasińska1, Guillermo Tenorio-Tagle2, Mónica Rodŕıguez2,
William J. Henney3
1 LUTH, Observatoire de Paris-Meudon, 5 Place Jules Jansen, 92195 Meudon, France
2 Instituto Nacional de Astrof́ısica Óptica y Electrónica, AP 51, 72000, Puebla, Mexico
3Centro de Radioastronomı́a y Astrof́ısica, Universidad Nacional Autónoma de México,
Campus Morelia, Apartado Postal 3-72, 58090 Morelia, Mexico
We argue that the discrepancies observed in HII regions between abundances derived from
optical recombination lines (ORLs) and collisionally excited lines (CELs) might well be the
signature of a scenario of the enrichment of the interstellar medium (ISM) proposed by Tenorio-
Tagle (1996). In this scenario, the fresh oxygen released during massive supernova explosions is
confined within the hot superbubbles as long as supernovae continue to explode. Only after the
last massive supernova explosion, the metal-rich gas starts cooling down and falls on the galaxy
within metal-rich droplets. Full mixing of these metal-rich droplets and the ISM occurs during
photoionization by the next generations of massive stars. During this process, the metal-rich
droplets give rise to strong recombination lines of the metals, leading to the observed ORL-CEL
discrepancy. (The full version of this work is submitted to Astronomy and Astrophysics.)
1. Introduction
There is no doubt that galaxies suffer chemical enrichment during their lives (see e.g.
Cid Fernandes et al. 2006 for a recent systematic approach using a large data base of
galaxies from the Sloan Digital Survey Data Release 5 – Adelman-Mac Carthy J.K. et
al., 2007). The main source of oxygen production has since long been identified as due
to supernovae from massive stars (type II supernovae). Yet, the exact process by which
chemical enrichment proceeds is poorly known (see a review by Scalo & Elmegreen 2004).
Ten years ago, Tenorio-Tagle (1996, hereafter T-T96) proposed a scenario in which the
metal-enhanced ejecta from supernovae follow a long excursion in galactic haloes before
falling down on the galaxies in the form of oxygen-rich droplets.
In the present work (the full version of which has been submitted to Astronomy &
Astrophysics, Stasińska et al. 2007), we suggest that the discrepancy between the oxygen
abundances derived from optical recombination lines (ORLs) and from collisionally ex-
cited lines (CELs) in HII regions (see e.g. Garćıa-Rojas et al. 2006 and references therein)
might well be the signature of those oxygen-rich droplets. In fact, Tsamis et al. (2003)
and Péquignot & Tsamis (2005) already suggested that the ORL/CEL discrepancy in
HII regions is the result of inhomegeneities in the chemical composition in these objects.
Our aim is to explicit the link between the ORL/CEL discrepancy and the T-T96 sce-
nario, and to check whether what is known of the oxygen yields allows one to explain
the ORL/CEL discrepancy in a quantitative way.
2. The Tenorio-Tagle (1996) scenario
Figures 1–5 present the T-T96 scenario in cartoon format.
http://arxiv.org/abs/0704.0160v1
2 Stasińska et al.: Oxygen-rich droplets and the enrichment of the ISM
Figure 1. Sketch of the T-T96 scenario: At time t=0, a burst of star formation occurs and a
giant HII region forms.
Figure 2. Sketch of the T-T96 scenario: During the next ∼ 40 Myr, supernovae explode, creating
a hot superbubble confined within a large expanding supershell that bursts into the galactic halo.
The superbubble contains the matter from the oxygen-rich supernova ejecta mixed with the
matter from the stellar winds and with the matter thermally evaporated from the surrounding
supershell.
3. The ORL-CEL discrepancy in the context of the T-T96 scenario
The details of the physical arguments concerning the amount of oxygen available in the
droplets, the mixing processes, as well as the simulation of the ORL-CEL discrepancy
with a multizone photoionization model are described in Stasińska et al. (2007). Here,
we simply give the most important conclusions.
Photoionization of the oxygen-rich droplets predicted by the T-T96 scenario can repro-
duce the observed abundance discrepancy factors (ADFs, i.e. the ratios of abundances
obtained from ORLs and from CELs) derived for Galactic and extragalactic HII regions.
The recombination lines arising from the highly metallic droplets thus show mixing at
work.
Stasińska et al.: Oxygen-rich droplets and the enrichment of the ISM 3
Figure 3. Sketch of the T-T96 scenario: after the last supernova has exploded, the gas in the
superbubble begins to cool down. Loci of higher densities cool down quicker. Due to a sequence
of fast repressurizing shocks, this leads to the formation of metal-rich cloudlets. The cooling
timescale is of the order of 100 Myr.
Figure 4. Sketch of the T-T96 scenario: The now cold metal-rich cloudlets fall unto the galactic
disk. They are further fragmented into metal-rich droplets by Raighleigh-Taylor instabilities.
This metal-rich rain affects a region whose extension is of the order of kiloparsecs, i.e. much
larger than the size of the initial HII region
We find that, if our scenario holds, the recombination lines strongly overestimate the
metallicities of the fully mixed HII regions. The collisionally excited lines may also over-
estimate them, although in much smaller proportion. In absence of any recipe to correct
for these biases, we recommend to discard objects showing large ADFs to probe the
chemical evolution of galaxies.
4 Stasińska et al.: Oxygen-rich droplets and the enrichment of the ISM
Figure 5. Sketch of the T-T96 scenario: When a next generation of massive stars form, they
photoionize the surrounding interstellar medium, including the metal-rich droplets. It is only
after the droplets have been photoionized that their matter is intimately mixed with the matter
from the ISM, and that proper chemical enrichment has occured. The whole process since the
explosion of the supernovae that provided fresh oxygen has taken at least 100 Myr.
To proceed further with this question of inhomogeneities, one needs as many observa-
tional constraints as possible.
On the theoretical side, one needs more robust estimates of the integrated stellar yields
as well as a better knowledge of the impact of massive stars on the ISM and of the role
of turbulence. All these issues are relevant to our understanding of the metal enrichment
of the Universe.
REFERENCES
Adelman-Mac Carthy J.K. et al., 2007, in preparation
Cid Fernandes, R., Vala Asari, N., Sodré Jr. L., Stasińska, G., Mateus, A., Torres-Papaqui, J.P.,
Schnoell, W., 2006, MNRAS in press (astro-ph/0610815)
Garćıa-Rojas, J., Esteban, C., Peimbert, M., Costado, M. T., Rodŕıguez, M., Peimbert, A., &
Ruiz, M. T. 2006, MNRAS, 368, 253
Scalo, J., & Elmegreen, B. G. 2004, ARA&A, 42, 275
Stasińska, G., Tenorio-Tagle, G., Rodŕıguez, M., Henney, W.J., 2007, A&A submitted
Tenorio-Tagle, G. 1996, AJ, 111, 1641 (T-T96)
Tsamis, Y. G., Barlow, M. J., Liu, X.-W., Danziger, I. J., & Storey, P. J. 2003, MNRAS, 338,
Tsamis, Y. G., & Péquignot, D. 2005, MNRAS, 364, 687
http://arxiv.org/abs/astro-ph/0610815
	Introduction
	The Tenorio-Tagle (1996) scenario
	The ORL-CEL discrepancy in the context of the T-T96 scenario
