Retention of Stellar-Mass Black Holes in Globular Clusters
Globular clusters should be born with significant numbers of stellar-mass black holes (BHs). It has been thought for two decades that very few of these BHs could be retained through the cluster lifetime. With masses ~10 MSun, BHs are ~20 times more massive than an average cluster star. They segregat...
Saved in:
Published in | arXiv.org |
---|---|
Main Authors | , , , |
Format | Paper Journal Article |
Language | English |
Published |
Ithaca
Cornell University Library, arXiv.org
02.02.2013
|
Subjects | |
Online Access | Get full text |
Cover
Loading…
Abstract | Globular clusters should be born with significant numbers of stellar-mass black holes (BHs). It has been thought for two decades that very few of these BHs could be retained through the cluster lifetime. With masses ~10 MSun, BHs are ~20 times more massive than an average cluster star. They segregate into the cluster core, where they may eventually decouple from the remainder of the cluster. The small-N core then evaporates on a short timescale. This is the so-called Spitzer instability. Here we present the results of a full dynamical simulation of a globular cluster containing many stellar-mass BHs with a realistic mass spectrum. Our Monte Carlo simulation code includes detailed treatments of all relevant stellar evolution and dynamical processes. Our main finding is that old globular clusters could still contain many BHs at present. In our simulation, we find no evidence for the Spitzer instability. Instead, most of the BHs remain well-mixed with the rest of the cluster, with only the innermost few tens of BHs segregating significantly. Over the 12 Gyr evolution, fewer than half of the BHs are dynamically ejected through strong binary interactions in the cluster core. The presence of BHs leads to long-term heating of the cluster, ultimately producing a core radius on the high end of the distribution for Milky Way globular clusters (and those of other galaxies). A crude extrapolation from our model suggests that the BH--BH merger rate from globular clusters could be comparable to the rate in the field. |
---|---|
AbstractList | Globular clusters should be born with significant numbers of stellar-mass black holes (BHs). It has been thought for two decades that very few of these BHs could be retained through the cluster lifetime. With masses ~10 MSun, BHs are ~20 times more massive than an average cluster star. They segregate into the cluster core, where they may eventually decouple from the remainder of the cluster. The small-N core then evaporates on a short timescale. This is the so-called Spitzer instability. Here we present the results of a full dynamical simulation of a globular cluster containing many stellar-mass BHs with a realistic mass spectrum. Our Monte Carlo simulation code includes detailed treatments of all relevant stellar evolution and dynamical processes. Our main finding is that old globular clusters could still contain many BHs at present. In our simulation, we find no evidence for the Spitzer instability. Instead, most of the BHs remain well-mixed with the rest of the cluster, with only the innermost few tens of BHs segregating significantly. Over the 12 Gyr evolution, fewer than half of the BHs are dynamically ejected through strong binary interactions in the cluster core. The presence of BHs leads to long-term heating of the cluster, ultimately producing a core radius on the high end of the distribution for Milky Way globular clusters (and those of other galaxies). A crude extrapolation from our model suggests that the BH--BH merger rate from globular clusters could be comparable to the rate in the field. 2013, ApJ, 763, L15 Globular clusters should be born with significant numbers of stellar-mass black holes (BHs). It has been thought for two decades that very few of these BHs could be retained through the cluster lifetime. With masses ~10 MSun, BHs are ~20 times more massive than an average cluster star. They segregate into the cluster core, where they may eventually decouple from the remainder of the cluster. The small-N core then evaporates on a short timescale. This is the so-called Spitzer instability. Here we present the results of a full dynamical simulation of a globular cluster containing many stellar-mass BHs with a realistic mass spectrum. Our Monte Carlo simulation code includes detailed treatments of all relevant stellar evolution and dynamical processes. Our main finding is that old globular clusters could still contain many BHs at present. In our simulation, we find no evidence for the Spitzer instability. Instead, most of the BHs remain well-mixed with the rest of the cluster, with only the innermost few tens of BHs segregating significantly. Over the 12 Gyr evolution, fewer than half of the BHs are dynamically ejected through strong binary interactions in the cluster core. The presence of BHs leads to long-term heating of the cluster, ultimately producing a core radius on the high end of the distribution for Milky Way globular clusters (and those of other galaxies). A crude extrapolation from our model suggests that the BH--BH merger rate from globular clusters could be comparable to the rate in the field. |
Author | Morscher, Meagan Umbreit, Stefan Rasio, Frederic A Farr, Will M |
Author_xml | – sequence: 1 givenname: Meagan surname: Morscher fullname: Morscher, Meagan – sequence: 2 givenname: Stefan surname: Umbreit fullname: Umbreit, Stefan – sequence: 3 givenname: Will surname: Farr middlename: M fullname: Farr, Will M – sequence: 4 givenname: Frederic surname: Rasio middlename: A fullname: Rasio, Frederic A |
BackLink | https://doi.org/10.1088/2041-8205/763/1/L15$$DView published paper (Access to full text may be restricted) https://doi.org/10.48550/arXiv.1211.3372$$DView paper in arXiv |
BookMark | eNotj89LwzAYhoMoOOfuniTguTU_-n3NvOmYmzARdPeStgl0xmQmreh_b-c8vYf35eF9LsipD94QcsVZXigAdqvjd_eVc8F5LmUpTshESMkzVQhxTmYp7RhjAksBICfk7tX0xvdd8DRY-tYb53TMnnVK9MHp5p2ugzOJdp6uXKiHsaQLN6TexHRJzqx2ycz-c0q2j8vtYp1tXlZPi_tNpoFDpuclQotNU9QlWl1jibVtWgSuDEhmrUEx1xLBQAmykIwBtkpw1K1pmKrllFwfsX9e1T52Hzr-VAe_6uA3Dm6Og30Mn4NJfbULQ_TjpUowJVAqNpJ_AZ0vUzU |
ContentType | Paper Journal Article |
Copyright | 2013. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License. http://arxiv.org/licenses/nonexclusive-distrib/1.0 |
Copyright_xml | – notice: 2013. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License. – notice: http://arxiv.org/licenses/nonexclusive-distrib/1.0 |
DBID | 8FE 8FG ABJCF ABUWG AFKRA AZQEC BENPR BGLVJ CCPQU DWQXO HCIFZ L6V M7S PIMPY PQEST PQQKQ PQUKI PRINS PTHSS GOX |
DOI | 10.48550/arxiv.1211.3372 |
DatabaseName | ProQuest SciTech Collection ProQuest Technology Collection Materials Science & Engineering Database (Proquest) ProQuest Central (Alumni) ProQuest Central UK/Ireland ProQuest Central Essentials AUTh Library subscriptions: ProQuest Central Technology Collection ProQuest One Community College ProQuest Central SciTech Premium Collection (Proquest) (PQ_SDU_P3) ProQuest Engineering Collection Engineering Database Access via ProQuest (Open Access) ProQuest One Academic Eastern Edition (DO NOT USE) ProQuest One Academic ProQuest One Academic UKI Edition ProQuest Central China Engineering Collection arXiv.org |
DatabaseTitle | Publicly Available Content Database Engineering Database Technology Collection ProQuest Central Essentials ProQuest One Academic Eastern Edition ProQuest Central (Alumni Edition) SciTech Premium Collection ProQuest One Community College ProQuest Technology Collection ProQuest SciTech Collection ProQuest Central China ProQuest Central ProQuest Engineering Collection ProQuest One Academic UKI Edition ProQuest Central Korea Materials Science & Engineering Collection ProQuest One Academic Engineering Collection |
DatabaseTitleList | Publicly Available Content Database |
Database_xml | – sequence: 1 dbid: GOX name: arXiv.org url: http://arxiv.org/find sourceTypes: Open Access Repository – sequence: 2 dbid: 8FG name: ProQuest Technology Collection url: https://search.proquest.com/technologycollection1 sourceTypes: Aggregation Database |
DeliveryMethod | fulltext_linktorsrc |
Discipline | Physics |
EISSN | 2331-8422 |
ExternalDocumentID | 1211_3372 |
Genre | Working Paper/Pre-Print |
GroupedDBID | 8FE 8FG ABJCF ABUWG AFKRA ALMA_UNASSIGNED_HOLDINGS AZQEC BENPR BGLVJ CCPQU DWQXO FRJ HCIFZ L6V M7S M~E PIMPY PQEST PQQKQ PQUKI PRINS PTHSS GOX |
ID | FETCH-LOGICAL-a515-a9765d6cc4b76fab676bfcd6518e530ffe629a365e5753430056d8216adec08b3 |
IEDL.DBID | GOX |
IngestDate | Mon Jan 08 05:44:01 EST 2024 Thu Oct 10 18:28:29 EDT 2024 |
IsDoiOpenAccess | true |
IsOpenAccess | true |
IsPeerReviewed | false |
IsScholarly | false |
Language | English |
LinkModel | DirectLink |
MergedId | FETCHMERGED-LOGICAL-a515-a9765d6cc4b76fab676bfcd6518e530ffe629a365e5753430056d8216adec08b3 |
OpenAccessLink | https://arxiv.org/abs/1211.3372 |
PQID | 2082638075 |
PQPubID | 2050157 |
ParticipantIDs | arxiv_primary_1211_3372 proquest_journals_2082638075 |
PublicationCentury | 2000 |
PublicationDate | 20130202 |
PublicationDateYYYYMMDD | 2013-02-02 |
PublicationDate_xml | – month: 02 year: 2013 text: 20130202 day: 02 |
PublicationDecade | 2010 |
PublicationPlace | Ithaca |
PublicationPlace_xml | – name: Ithaca |
PublicationTitle | arXiv.org |
PublicationYear | 2013 |
Publisher | Cornell University Library, arXiv.org |
Publisher_xml | – name: Cornell University Library, arXiv.org |
SSID | ssj0002672553 |
Score | 1.5407321 |
SecondaryResourceType | preprint |
Snippet | Globular clusters should be born with significant numbers of stellar-mass black holes (BHs). It has been thought for two decades that very few of these BHs... 2013, ApJ, 763, L15 Globular clusters should be born with significant numbers of stellar-mass black holes (BHs). It has been thought for two decades that very... |
SourceID | arxiv proquest |
SourceType | Open Access Repository Aggregation Database |
SubjectTerms | Binary stars Black holes Computer simulation Dynamic stability Galaxies Galaxy distribution Globular clusters Milky Way Monte Carlo simulation Physics - Astrophysics of Galaxies Stellar evolution |
SummonAdditionalLinks | – databaseName: ProQuest Technology Collection dbid: 8FG link: http://utb.summon.serialssolutions.com/2.0.0/link/0/eLvHCXMwfV1NSwMxEA3aInjz22qVHLxGm00yu_XioViLoIhW6G3JJwjS1t1W_Plm0q0eBGFP2VNewszL5OUNIRdOuZhUQLFgQDJpXM5Mv3DM8ABK6SKmoCSQfYTRq7yfqElTcKsbWeU6JqZA7WYWa-TxkB6JMLqjq5v5B8OuUXi72rTQ2CRtjk54-FJ8ePdTY8kgj4xZrG4nk3XXla6-3j7RUoFfCoG2wO008icSp_Qy3CHtJz331S7Z8NM9spVUmbbeJ9fPSGkROjoL9AUffOiKPUS-S1PhjY7Qjom-TSmKJlBQSgfvS7Q-qA_IeHg7HoxY0-yA6UgpmI60QDmwVpocgjaQgwnWgeKFV6IXgoesrwUoH_mVkGgyD67IOGjnba8w4pC0prOpPyZURMJsDXArMy699Sb0vZPGewmZtJZ3yFGaczlf-VmUiEaJaHRId41C2WzluvwF_uT_36dkO0u9IrL4dUlrUS39WczYC3OeluUb7oKUpg priority: 102 providerName: ProQuest |
Title | Retention of Stellar-Mass Black Holes in Globular Clusters |
URI | https://www.proquest.com/docview/2082638075 https://arxiv.org/abs/1211.3372 |
hasFullText | 1 |
inHoldings | 1 |
isFullTextHit | |
isPrint | |
link | http://utb.summon.serialssolutions.com/2.0.0/link/0/eLvHCXMwdV1LSwMxEB5qvXgRxVe11hy8RrvZZHbrTUsfCK1SK_S25AkFqdKHePK3m2S3XkQIOYTkkEmY70sy-Qbg2gjjQQUFdQo55cpkVHVyQ1XiUAiZewiKAbJjHL7yx5mY1eBq-xdGLr_mn6U-sFrdBv2xmzTNvI_dYSxEbA2eZuVjY1Tiqrr_dvMMM7b8cawRLfoHsF_RPHJfrssh1OziCO4mgaEGS5B3R17C_w25pCNPX0m8RyPDoK5E5gsSYiBCfCjpvm2CksHqGKb93rQ7pFXuAio9Q6DSo7wwqDVXGTqpMEPltEGR5Fakbecsso5MUVhPl1IeNOPR5CxBaaxu5yo9gbo__tszIKnnv1phojlLuNVWuY41XFnLkXGtkwacxjkXH6U8RRGsUQRrNKC5tUJR7cxVwTzmY1CZF-f_DryAPRazPjBfmlBfLzf20mPvWrVgJ-8PWrD70Bs_T1pxPXw9-u79AAt3h0E |
link.rule.ids | 228,230,786,790,891,12792,21416,27956,33406,33777,43633,43838 |
linkProvider | Cornell University |
linkToHtml | http://utb.summon.serialssolutions.com/2.0.0/link/0/eLvHCXMwfV09T8MwELWgFYKNbwoFMrAaSGxfUhaGihKgrRAUqVvkr0iVUFqSFvHz8bkpDEhImZzJz9bd8_n5HSEXRhiXVEDQXAGnXJmYqk5iqApzEEImLgV5gewQ0jf-OBbjuuBW1bLKVUz0gdpMNdbI3SHdEWF0Rxe3sw-KXaPwdrVuobFOmpwBw32e9O5_aiwRxI4xs-XtpLfuupLl1-QTLRXCS8bQFrjpR_5EYp9eetuk-Sxnttwha7bYJRtelamrPXLzgpQWoQumefCKDz5kSQeO7wa-8BakaMcUTIoARRMoKA267wu0Pqj2yah3N-qmtG52QKWjFFQ6WiAMaM1VDLlUEIPKtQERJlaw6zy3EHUkA2Edv2IcTebBJFEI0lh9nSh2QBrFtLBHJGCOMGsFoeZRyK22Ku9Yw5W1HCKuddgih37O2WzpZ5EhGhmi0SLtFQpZvZWr7Bf44_9_n5PNdDToZ_2H4dMJ2Yp834jIfW3SmJcLe-qy91yd-SX6BgWjl44 |
openUrl | ctx_ver=Z39.88-2004&ctx_enc=info%3Aofi%2Fenc%3AUTF-8&rfr_id=info%3Asid%2Fsummon.serialssolutions.com&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.atitle=Retention+of+Stellar-Mass+Black+Holes+in+Globular+Clusters&rft.jtitle=arXiv.org&rft.au=Morscher%2C+Meagan&rft.au=Umbreit%2C+Stefan&rft.au=Farr%2C+Will+M&rft.au=Rasio%2C+Frederic+A&rft.date=2013-02-02&rft.pub=Cornell+University+Library%2C+arXiv.org&rft.eissn=2331-8422&rft_id=info:doi/10.48550%2Farxiv.1211.3372 |