The Galactic underworld: the spatial distribution of compact remnants
ABSTRACT We chart the expected Galactic distribution of neutron stars and black holes. These compact remnants of dead stars – the Galactic underworld – are found to exhibit a fundamentally different distribution and structure to the visible Galaxy. Compared to the visible Galaxy, concentration into...
Gespeichert in:
Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2022-09, Vol.516 (4), p.4971-4979 |
---|---|
Hauptverfasser: | , , , |
Format: | Artikel |
Sprache: | eng |
Online-Zugang: | Volltext bestellen |
Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
container_end_page | 4979 |
---|---|
container_issue | 4 |
container_start_page | 4971 |
container_title | Monthly notices of the Royal Astronomical Society |
container_volume | 516 |
creator | Sweeney, David Tuthill, Peter Sharma, Sanjib Hirai, Ryosuke |
description | ABSTRACT
We chart the expected Galactic distribution of neutron stars and black holes. These compact remnants of dead stars – the Galactic underworld – are found to exhibit a fundamentally different distribution and structure to the visible Galaxy. Compared to the visible Galaxy, concentration into a thin flattened disc structure is much less evident with the scale height more than tripling to 1260 ± 30 pc. This difference arises from two primary causes. First, the distribution is in part inherited from the integration over the evolving structure of the Galaxy itself (and hence the changing distribution of the parent stars). Secondly, an even larger effect arises from the natal kick received by the remnant at the event of its supernova birth. Due to this kick we find 30 per cent of remnants have sufficient kinetic energy to entirely escape the Galactic potential (40 per cent of neutron stars and 2 per cent of black holes) leading to a Galactic mass-loss integrated to the present day of $\sim 0.4{{\ \rm per\ cent}}$ of the stellar mass of the Galaxy. The black hole – neutron star fraction increases near the Galactic centre: a consequence of smaller kick velocities in the former. Our simulated remnant distribution yields probable distances of 19 and 21 pc to the nearest neutron star and black hole, respectively, while our nearest probable magnetar lies at 4.2 kpc. Although the underworld only contains of order $\sim 1{{\ \rm per\ cent}}$ of the Galaxy’s mass, observational signatures and physical traces of its population, such as microlensing, will become increasingly present in data ranging from gravitational wave detectors to high precision surveys from space missions such as Gaia. |
doi_str_mv | 10.1093/mnras/stac2092 |
format | Article |
fullrecord | <record><control><sourceid>oup_TOX</sourceid><recordid>TN_cdi_crossref_primary_10_1093_mnras_stac2092</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><oup_id>10.1093/mnras/stac2092</oup_id><sourcerecordid>10.1093/mnras/stac2092</sourcerecordid><originalsourceid>FETCH-LOGICAL-c273t-16815049a80ee8995d4ea809ee1fd85ecb9cd6e9c18cf30e04ace1ae465b765b3</originalsourceid><addsrcrecordid>eNqFkDFPwzAQRi0EEqGwMntlSHuOY8dmQ1UpSJVYyhw5zkUYJXFkO0L8ewKFmeH0nXT3vuERcstgzUDzzTAGEzcxGVuALs5IxrgUeaGlPCcZABe5qhi7JFcxvgNAyQuZkd3xDene9MYmZ-k8thg-fOjbe5qWQ5xMcqanrYspuGZOzo_Ud9T6YVoIGnAYzZjiNbnoTB_x5jdX5PVxd9w-5YeX_fP24ZDbouIpZ1IxAaU2ChCV1qItcdk1IutaJdA22rYStWXKdhwQSmORGSylaKpl-IqsT702-BgDdvUU3GDCZ82g_pZQ_0io_yQswN0J8PP03-8XfLZhsg</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype></control><display><type>article</type><title>The Galactic underworld: the spatial distribution of compact remnants</title><source>Oxford Journals Open Access Collection</source><creator>Sweeney, David ; Tuthill, Peter ; Sharma, Sanjib ; Hirai, Ryosuke</creator><creatorcontrib>Sweeney, David ; Tuthill, Peter ; Sharma, Sanjib ; Hirai, Ryosuke</creatorcontrib><description>ABSTRACT
We chart the expected Galactic distribution of neutron stars and black holes. These compact remnants of dead stars – the Galactic underworld – are found to exhibit a fundamentally different distribution and structure to the visible Galaxy. Compared to the visible Galaxy, concentration into a thin flattened disc structure is much less evident with the scale height more than tripling to 1260 ± 30 pc. This difference arises from two primary causes. First, the distribution is in part inherited from the integration over the evolving structure of the Galaxy itself (and hence the changing distribution of the parent stars). Secondly, an even larger effect arises from the natal kick received by the remnant at the event of its supernova birth. Due to this kick we find 30 per cent of remnants have sufficient kinetic energy to entirely escape the Galactic potential (40 per cent of neutron stars and 2 per cent of black holes) leading to a Galactic mass-loss integrated to the present day of $\sim 0.4{{\ \rm per\ cent}}$ of the stellar mass of the Galaxy. The black hole – neutron star fraction increases near the Galactic centre: a consequence of smaller kick velocities in the former. Our simulated remnant distribution yields probable distances of 19 and 21 pc to the nearest neutron star and black hole, respectively, while our nearest probable magnetar lies at 4.2 kpc. Although the underworld only contains of order $\sim 1{{\ \rm per\ cent}}$ of the Galaxy’s mass, observational signatures and physical traces of its population, such as microlensing, will become increasingly present in data ranging from gravitational wave detectors to high precision surveys from space missions such as Gaia.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stac2092</identifier><language>eng</language><publisher>Oxford University Press</publisher><ispartof>Monthly notices of the Royal Astronomical Society, 2022-09, Vol.516 (4), p.4971-4979</ispartof><rights>2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society 2022</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c273t-16815049a80ee8995d4ea809ee1fd85ecb9cd6e9c18cf30e04ace1ae465b765b3</citedby><cites>FETCH-LOGICAL-c273t-16815049a80ee8995d4ea809ee1fd85ecb9cd6e9c18cf30e04ace1ae465b765b3</cites><orcidid>0000-0002-8032-8174 ; 0000-0002-7528-1463</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,1598,27901,27902</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/stac2092$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Sweeney, David</creatorcontrib><creatorcontrib>Tuthill, Peter</creatorcontrib><creatorcontrib>Sharma, Sanjib</creatorcontrib><creatorcontrib>Hirai, Ryosuke</creatorcontrib><title>The Galactic underworld: the spatial distribution of compact remnants</title><title>Monthly notices of the Royal Astronomical Society</title><description>ABSTRACT
We chart the expected Galactic distribution of neutron stars and black holes. These compact remnants of dead stars – the Galactic underworld – are found to exhibit a fundamentally different distribution and structure to the visible Galaxy. Compared to the visible Galaxy, concentration into a thin flattened disc structure is much less evident with the scale height more than tripling to 1260 ± 30 pc. This difference arises from two primary causes. First, the distribution is in part inherited from the integration over the evolving structure of the Galaxy itself (and hence the changing distribution of the parent stars). Secondly, an even larger effect arises from the natal kick received by the remnant at the event of its supernova birth. Due to this kick we find 30 per cent of remnants have sufficient kinetic energy to entirely escape the Galactic potential (40 per cent of neutron stars and 2 per cent of black holes) leading to a Galactic mass-loss integrated to the present day of $\sim 0.4{{\ \rm per\ cent}}$ of the stellar mass of the Galaxy. The black hole – neutron star fraction increases near the Galactic centre: a consequence of smaller kick velocities in the former. Our simulated remnant distribution yields probable distances of 19 and 21 pc to the nearest neutron star and black hole, respectively, while our nearest probable magnetar lies at 4.2 kpc. Although the underworld only contains of order $\sim 1{{\ \rm per\ cent}}$ of the Galaxy’s mass, observational signatures and physical traces of its population, such as microlensing, will become increasingly present in data ranging from gravitational wave detectors to high precision surveys from space missions such as Gaia.</description><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><recordid>eNqFkDFPwzAQRi0EEqGwMntlSHuOY8dmQ1UpSJVYyhw5zkUYJXFkO0L8ewKFmeH0nXT3vuERcstgzUDzzTAGEzcxGVuALs5IxrgUeaGlPCcZABe5qhi7JFcxvgNAyQuZkd3xDene9MYmZ-k8thg-fOjbe5qWQ5xMcqanrYspuGZOzo_Ud9T6YVoIGnAYzZjiNbnoTB_x5jdX5PVxd9w-5YeX_fP24ZDbouIpZ1IxAaU2ChCV1qItcdk1IutaJdA22rYStWXKdhwQSmORGSylaKpl-IqsT702-BgDdvUU3GDCZ82g_pZQ_0io_yQswN0J8PP03-8XfLZhsg</recordid><startdate>20220930</startdate><enddate>20220930</enddate><creator>Sweeney, David</creator><creator>Tuthill, Peter</creator><creator>Sharma, Sanjib</creator><creator>Hirai, Ryosuke</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><orcidid>https://orcid.org/0000-0002-8032-8174</orcidid><orcidid>https://orcid.org/0000-0002-7528-1463</orcidid></search><sort><creationdate>20220930</creationdate><title>The Galactic underworld: the spatial distribution of compact remnants</title><author>Sweeney, David ; Tuthill, Peter ; Sharma, Sanjib ; Hirai, Ryosuke</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c273t-16815049a80ee8995d4ea809ee1fd85ecb9cd6e9c18cf30e04ace1ae465b765b3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Sweeney, David</creatorcontrib><creatorcontrib>Tuthill, Peter</creatorcontrib><creatorcontrib>Sharma, Sanjib</creatorcontrib><creatorcontrib>Hirai, Ryosuke</creatorcontrib><collection>CrossRef</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Sweeney, David</au><au>Tuthill, Peter</au><au>Sharma, Sanjib</au><au>Hirai, Ryosuke</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The Galactic underworld: the spatial distribution of compact remnants</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2022-09-30</date><risdate>2022</risdate><volume>516</volume><issue>4</issue><spage>4971</spage><epage>4979</epage><pages>4971-4979</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>ABSTRACT
We chart the expected Galactic distribution of neutron stars and black holes. These compact remnants of dead stars – the Galactic underworld – are found to exhibit a fundamentally different distribution and structure to the visible Galaxy. Compared to the visible Galaxy, concentration into a thin flattened disc structure is much less evident with the scale height more than tripling to 1260 ± 30 pc. This difference arises from two primary causes. First, the distribution is in part inherited from the integration over the evolving structure of the Galaxy itself (and hence the changing distribution of the parent stars). Secondly, an even larger effect arises from the natal kick received by the remnant at the event of its supernova birth. Due to this kick we find 30 per cent of remnants have sufficient kinetic energy to entirely escape the Galactic potential (40 per cent of neutron stars and 2 per cent of black holes) leading to a Galactic mass-loss integrated to the present day of $\sim 0.4{{\ \rm per\ cent}}$ of the stellar mass of the Galaxy. The black hole – neutron star fraction increases near the Galactic centre: a consequence of smaller kick velocities in the former. Our simulated remnant distribution yields probable distances of 19 and 21 pc to the nearest neutron star and black hole, respectively, while our nearest probable magnetar lies at 4.2 kpc. Although the underworld only contains of order $\sim 1{{\ \rm per\ cent}}$ of the Galaxy’s mass, observational signatures and physical traces of its population, such as microlensing, will become increasingly present in data ranging from gravitational wave detectors to high precision surveys from space missions such as Gaia.</abstract><pub>Oxford University Press</pub><doi>10.1093/mnras/stac2092</doi><tpages>9</tpages><orcidid>https://orcid.org/0000-0002-8032-8174</orcidid><orcidid>https://orcid.org/0000-0002-7528-1463</orcidid></addata></record> |
fulltext | fulltext_linktorsrc |
identifier | ISSN: 0035-8711 |
ispartof | Monthly notices of the Royal Astronomical Society, 2022-09, Vol.516 (4), p.4971-4979 |
issn | 0035-8711 1365-2966 |
language | eng |
recordid | cdi_crossref_primary_10_1093_mnras_stac2092 |
source | Oxford Journals Open Access Collection |
title | The Galactic underworld: the spatial distribution of compact remnants |
url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-02-05T10%3A02%3A16IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-oup_TOX&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=The%20Galactic%20underworld:%20the%20spatial%20distribution%20of%20compact%20remnants&rft.jtitle=Monthly%20notices%20of%20the%20Royal%20Astronomical%20Society&rft.au=Sweeney,%20David&rft.date=2022-09-30&rft.volume=516&rft.issue=4&rft.spage=4971&rft.epage=4979&rft.pages=4971-4979&rft.issn=0035-8711&rft.eissn=1365-2966&rft_id=info:doi/10.1093/mnras/stac2092&rft_dat=%3Coup_TOX%3E10.1093/mnras/stac2092%3C/oup_TOX%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_id=info:pmid/&rft_oup_id=10.1093/mnras/stac2092&rfr_iscdi=true |