Nova-driven winds in globular clusters

Scott, E. H.; Durisen, R. H.

doi:10.1086/156177

Cited by 24 publications

(23 citation statements)

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“…The least-frequent mechanism may be stellar collisions (Umbreit et al 2008), which would be too infrequent to account for ICM clearing on timescales much shorter than every ∼10 6 years. Scott & Durisen (1978) proposed novae as a clearing mechanism and, while dwarf novae seem to be rare (e.g. Servillat et al 2011), they may be a plausible mechanism for small clusters (Moore & Bildsten 2011).…”

Section: Energy Sources For Clearing Clustersmentioning

confidence: 98%

Globular cluster interstellar media: ionized and ejected by white dwarfs

McDonald¹,

Zijlstra²

2014

Monthly Notices of the Royal Astronomical Society

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UV radiation from white dwarfs can efficiently clear Galactic globular clusters (GCs) of their intra-cluster medium (ICM). This solves the problem of the missing ICM in clusters, which is otherwise expected to build up to easily observable quantities. To show this, we recreate the ionizing flux in 47 Tuc, following randomly generated stars through their AGB, post-AGB and white dwarf evolution. Each white dwarf can ionize all the material injected into the cluster by stellar winds for ∼3 Myr of its evolution: ∼40 such white dwarfs exist at any point. Every GC's ICM should be ionized. The neutral cloud in M15 should be caused by a temporary overdensity. A pressure-supported ICM will expand over the cluster's tidal radius, where it will be truncated, allowing Jeans escape. The modelled Jeans mass-loss rate approximates the total stellar mass-loss rate, allowing efficient clearing of ICM. Any cluster's ICM mass should equal the mass injected by its stars over the sound-travel time between the cluster core and tidal radius. We predict ∼11.3 M ⊙ of ICM within 47 Tuc, cleared over ∼4 Myr, compared to a dynamical timescale of 4.3 Myr. We present a new mass hierarchy, discussing the transition between globular clusters dwarf galaxies.

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Section: Energy Sources For Clearing Clustersmentioning

confidence: 98%

Globular cluster interstellar media: ionized and ejected by white dwarfs

McDonald¹,

Zijlstra²

2014

Monthly Notices of the Royal Astronomical Society

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“…M15) where the shell escape time, t esc , is so long that it does not escape before another CN occurs. The outcomes from these colliding remnants are more complex, either leading to a net heating of the ICM that creates a wind like solution (Scott & Durisen 1978) or more intense cooling that keeps the material bound. In either case, novae clearing is most effective in the smaller, less dense clusters, where the shell safely escapes before another nova goes off and the GC is in no danger of a runaway scenario.…”

Section: Application To Galactic Clustersmentioning

confidence: 99%

“…We have reconsidered the Scott & Durisen (1978) model of using CNe explosions to clear the accumulated ICM in galactic GCs, allowing for a more secure analysis of its efficacy. Using estimated CNe rates and the known stellar mass loss rates, we predict that novae clearing is highly effective in the less massive and less centrally condensed galactic GCs (those unlikely to undergo a runaway), leading to a typical ICM buildup of ≈ 0.03M that is consistent with observational upper limits.…”

Section: Conclusion and Other Applicationsmentioning

confidence: 99%

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

Moore¹,

Bildsten²

2011

ApJ

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Observations of the intra-cluster medium (ICM) in galactic globular clusters (GCs) show a systematic deficiency in ICM mass as compared to that expected from accumulation of stellar winds in the time available between galactic plane crossings. In this paper, we reexamine the original hypothesis of Scott and Durisen that hydrogen-rich explosions on accreting white dwarfs, classical novae (CNe), will sweep out the ICM from the cluster more frequently than galactic plane crossings. From the CNe rate and stellar mass-loss rate, this clearing mechanism predicts that ≈ 0.03 M should be present in ≤ 10 5 M GCs. We model the expanding remnant made from the 10 −4 M nova ejecta and show that it escapes long before it has cooled. We discuss the few positive ICM measurements and use a Monte-Carlo simulation of the accumulation and CNe recurrence times to reveal the possible variance in the ICM masses for the higher mass (> 5 × 10 5 M ) GCs. We find that nova shells are effective at clearing the ICM in low-mass GCs (≤ 10 5 M ), whereas higher-mass clusters may experience a quiescent time between novae long enough to prevent the next nova shell from escaping. The nova clearing mechanism will also operate in ultra-faint Milky Way satellites, where many upper limits on gas masses are available.

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“…There is strong observational and theoretical evidence that stars reaching the AGB phase lose a large amount of mass. Several studies have been devoted to the fate of this gas in clusters (Scott & Rose 1975;Faulkner & Freeman 1977;Vandenberg & Faulkner 1977;Vandenberg 1978;Scott & Durisen 1978;Faulkner 1984;Faulkner & Coleman 1984;Smith 1996). Stellar ejecta in GCs with shallow potential wells can leave the cluster via a smooth wind-like outflow.…”

Section: Introductionmentioning

confidence: 99%

Accretion of gas by globular cluster stars

Thoul

Jorissen

Goriely

et al. 2002

A&A

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Abstract. Some recent observations of the abundances of s-process, r-process, and α elements in metal-poor stars have led to a new scenario for their formation. According to this scenario, these stars were born in a globular cluster and accreted the s-process enriched gas expelled by cluster stars of higher-mass, thereby modifying their surface abundances. Later on, these polluted stars evaporated from the globular cluster to constitute an important fraction of the current halo population. In addition, there are now many direct observations of abundance anomalies not only in globular cluster giant stars but also in subgiant and main-sequence stars. Accretion again provides a plausible explanation for (at least some of) these peculiarities. Here we investigate further the efficiency of the accretion scenario. We find that in concentrated clusters with large escape velocities, accretion is very efficient and can indeed lead to major modifications of the stellar surface abundances.

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Nova-driven winds in globular clusters

Cited by 24 publications

References 0 publications

Globular cluster interstellar media: ionized and ejected by white dwarfs

Globular cluster interstellar media: ionized and ejected by white dwarfs

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

Accretion of gas by globular cluster stars

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