Clearing the Gas From Globular Clusters and Dwarf Spheroidals With Classical Novae

Moore, Kevin L.; Bildsten, Lars

doi:10.1088/0004-637x/728/2/81

Cited by 20 publications

(22 citation statements)

References 68 publications

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“…2, we obtain the tightest H I constraints for nearby, unresolved (N b = 1) systems, which probe how gas is recycled into the interstellar medium (ISM) of the dSphs themselves. Assuming that a lowmass star in an old (> 10 Gyr) stellar population losses ∼ 0.3 M ⊙ of material after turning off the main sequence, Moore & Bildsten (2011) estimate a mass loss rate oḟ…”

Section: Discussionmentioning

confidence: 99%

The Dearth of Neutral Hydrogen in Galactic Dwarf Spheroidal Galaxies

Spekkens¹,

Urbancic²,

Mason³

et al. 2014

ApJ

158

173

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We present new upper limits on the neutral hydrogen (H I) content within the stellar half-light ellipses of 15 Galactic dwarf spheroidal galaxies (dSphs), derived from pointed observations with the Green Bank Telescope (GBT) as well as Arecibo L-band Fast ALFA (ALFALFA) survey and Galactic All-Sky Survey (GASS) data. All of the limits M lim HI are more stringent than previously reported values, and those from the GBT improve upon contraints in the literature by a median factor of 23.−5 , irrespective of location in the Galactic halo. Comparing these relative H I contents to those of the Local Group and nearby neighbor dwarfs compiled by McConnachie, we find that the Galactic dSphs are extremely gas-poor. Our H I upper limits therefore provide the clearest picture yet of the environmental dependence of the H I content in Local Volume dwarfs. If ram pressure stripping explains the dearth of H I in these systems, then orbits in a relatively massive Milky Way are favored for the outer halo dSph Leo I, while Leo II and Canes Venatici I have had a pericentric passage in the past. For Draco and Ursa Minor, the interstellar medium mass that should accumulate through stellar mass loss in between pericentric passages exceeds M lim HI by a factor of ∼ 30. In Ursa Minor, this implies that either this material is not in the atomic phase, or that another mechanism clears the recycled gas on shorter timescales.

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Section: Discussionmentioning

confidence: 99%

The Dearth of Neutral Hydrogen in Galactic Dwarf Spheroidal Galaxies

Spekkens¹,

Urbancic²,

Mason³

et al. 2014

ApJ

158

173

View full text Add to dashboard Cite

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“…The physics of NSCs in galaxies, namely, their origin, history and the composition of their interstellar environment has a close re-semblance on smaller scales to the properties of globular clusters (de Grijs & Lépine 2010). Unlike nuclei of galaxies, typical globular clusters lack SMBHs in their cores; also, they are generally unable to retain any significant amount of gas and dust (Frank & Gisler 1976;Moore & Bildsten 2011). However, the category of Ultra-Compact Dwarf galaxies (Mieske et al 2013;Mieske 2014) appears to be a suitable type of object that can help us to explore the physics and evolution of NSCs with a central SMBH, and to compare them with the properties of the NSC in our Galaxy.…”

Section: Introductionmentioning

confidence: 99%

Multiphase environment of compact galactic nuclei: the role of the nuclear star cluster

Różáńska

Kunneriath

Adhikari

et al. 2016

Mon. Not. R. Astron. Soc.

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We study the conditions for the onset of Thermal Instability in the innermost regions of compact galactic nuclei, where the properties of the interstellar environment are governed by the interplay of quasi-spherical accretion onto a supermassive black hole (SMBH) and the heating/cooling processes of gas in a dense nuclear star cluster. Stellar winds are the source of material for radiatively inefficient (quasi-spherical, non-magnetised) inflow/outflow onto the central SMBH, where a stagnation point develops within the Bondi type accretion. We study the local thermal equilibrium to determine the parameter space which allows cold and hot phases in mutual contact to co-exist. We include the effects of mechanical heating by stellar winds and radiative cooling/heating by the ambient field of the dense star cluster. We consider two examples: the Nuclear Star Cluster (NSC) in the Milky Way central region (including the gaseous Mini-spiral of Sgr A*), and the Ultra-Compact Dwarf galaxy M60-UCD1. We find that the two systems behave in different ways because they are placed in different areas of parameter space in the instability diagram: gas temperature vs. dynamical ionization parameter. In the case of Sgr A*, stellar heating prevents the spontaneous formation of cold clouds. The plasma from stellar winds joins the hot X-ray emitting phase and forms an outflow. In M60-UCD1 our model predicts spontaneous formation of cold clouds in the inner part of the galaxy. These cold clouds may survive since the cooling timescale is shorter than the inflow/outflow timescale.

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“…Vanbeveren, van Bever & De Donder 1997; Vanbeveren, De Loore & Van Rensbergen 1998; Belkus et al 2003; Zhang et al 2005; Dionne & Robert 2006; Han, Podsiadlowski & Lynas‐Gray 2007; Eldridge & Stanway 2009). The potential effect on galactic structure of a subset of compact binaries other than XBs has also recently been considered by Moore & Bildsten (2011); binary stars matter on galactic scales.…”

Section: Introductionmentioning

confidence: 99%

Another thread in the tapestry of stellar feedback: X-ray binaries

Justham

Schawinski

2012

Monthly Notices of the Royal Astronomical Society

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We consider X-ray binaries (XBs) as potential sources of stellar feedback. XBs observationally appear able to deposit a high fraction of their power output into their local interstellar medium, which may make them a non-negligible source of energy input. The formation rate of the most luminous XBs rises with decreasing metallicity, which should increase their significance during galaxy formation in the early universe. We also argue that stochastic effects are important to XB feedback (XBF) and may dominate the systematic changes due to metallicity in many cases. Large stochastic variation in the magnitude of XBF at low absolute star formation rates provides a natural reason for diversity in the evolution of dwarf galaxies which were initially almost identical, with several percent of such halos experiencing energy input from XBs roughly two orders of magnitude above the most likely value. These probability distributions suggest that the effect of XBF is most commonly significant for total stellar masses between ~10^7 and 10^8 Msun, which might resolve a current problem with modelling populations of such galaxies. We explain how XBs might inject energy before luminous supernovae (SNe) contribute significantly to feedback and how XBs can assist in keeping gas hot long after the last core-collapse SN has exploded. [...] XBF could be especially important to some dwarf galaxies, potentially heating gas without expelling it; the properties of XBF also match those previously derived as allowing episodic star formation. We also argue that the efficiency of SN feedback (SNF) might be reduced when XBF has had the opportunity to act first. In addition, we note that the effect of SNF is unlikely to be scale-free; galaxies smaller than ~100 pc might well experience less effective SNF. (Slightly abbreviated to fit arXiv size limit.)Comment: Very belatedly updated to include a note added in proof and additional reference. The definitive version is at: mnras.oxfordjournals.org/content/423/2/164

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Clearing the Gas From Globular Clusters and Dwarf Spheroidals With Classical Novae

Cited by 20 publications

References 68 publications

The Dearth of Neutral Hydrogen in Galactic Dwarf Spheroidal Galaxies

The Dearth of Neutral Hydrogen in Galactic Dwarf Spheroidal Galaxies

Multiphase environment of compact galactic nuclei: the role of the nuclear star cluster

Another thread in the tapestry of stellar feedback: X-ray binaries

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