Cloud Formation by Supernova Implosion
The deposition of energy and momentum by supernova explosions has been subject to numerous studies in the past few decades. However, while there has been some work that focused on the transition from the adiabatic to the radiative stage of a supernova remnant (SNR), the late radiative stage and merg...
Gespeichert in:
Veröffentlicht in: | The Astrophysical journal 2024-04, Vol.965 (2), p.168 |
---|---|
Hauptverfasser: | , , |
Format: | Artikel |
Sprache: | eng |
Schlagworte: | |
Online-Zugang: | Volltext |
Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
container_end_page | |
---|---|
container_issue | 2 |
container_start_page | 168 |
container_title | The Astrophysical journal |
container_volume | 965 |
creator | Romano, Leonard E. C. Behrendt, Manuel Burkert, Andreas |
description | The deposition of energy and momentum by supernova explosions has been subject to numerous studies in the past few decades. However, while there has been some work that focused on the transition from the adiabatic to the radiative stage of a supernova remnant (SNR), the late radiative stage and merging with the interstellar medium (ISM) have received little attention. Here, we use three-dimensional, hydrodynamic simulations, focusing on the evolution of SNRs during the radiative phase, considering a wide range of physical explosion parameters (
n
H
,
ISM
∈
0.1
,
100
cm
−
3
and
E
SN
∈
1
,
14
×
10
51
erg
). We find that the radiative phase can be subdivided in four stages: A pressure-driven snowplow phase, during which the hot overpressurized bubble gas is evacuated and pushed into the cold shell; a momentum-conserving snowplow phase that is accompanied by a broadening of the shell; an implosion phase where cold material from the back of the shell is flooding the central vacuum; and a final cloud phase, during which the imploding gas is settling as a central, compact overdensity. The launching timescale for the implosion ranges from a few 100 kyr to a few Myr, while the cloud formation timescale ranges from a few to about 10 Myr. The highly chemically enriched clouds can become massive (
M
cl
∼ 10
3
–10
4
M
⊙
) and self-gravitating within a few Myr after their formation, providing an attractive, novel pathway for supernova-induced star and planet formation in the ISM. |
doi_str_mv | 10.3847/1538-4357/ad2c05 |
format | Article |
fullrecord | <record><control><sourceid>proquest_cross</sourceid><recordid>TN_cdi_crossref_primary_10_3847_1538_4357_ad2c05</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><doaj_id>oai_doaj_org_article_66dfdc4bb80c4dd0b81f30178fded153</doaj_id><sourcerecordid>3040595508</sourcerecordid><originalsourceid>FETCH-LOGICAL-c399t-f764046e76f0d5598f4e40802417731fec61af1b3519d3457f7eced3e4123a0f3</originalsourceid><addsrcrecordid>eNp9kM1LxDAQxYMouK7ePRZET9adNN9HWVxdEDyo4C2kTSIt3U1NW2H_e1sr60U8DfN482bmh9A5hhsiqVhgRmRKCRMLY7MC2AGa7aVDNAMAmnIi3o7RSdtWY5spNUNXyzr0NlmFuDFdGbZJvkue-8bFbfg0yXrT1KEd5FN05E3durOfOkevq7uX5UP6-HS_Xt4-pgVRqku94BQod4J7sIwp6amjICGjWAiCvSs4Nh7nhGFlCWXCC1c4SxzFGTHgyRytp1wbTKWbWG5M3OlgSv0thPiuTezKonaac-ttQfNcQkGthVxiTwAL6a2zw-tD1sWU1cTw0bu201Xo43Y4XxOgwBRjIAcXTK4ihraNzu-3YtAjWT1i1CNGPZEdRq6nkTI0v5n_2C__sJum0ooznWnMpW6sJ1-NTIR-</addsrcrecordid><sourcetype>Open Website</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>3040595508</pqid></control><display><type>article</type><title>Cloud Formation by Supernova Implosion</title><source>Open Access: IOP Publishing Free Content</source><source>DOAJ Directory of Open Access Journals</source><source>Alma/SFX Local Collection</source><source>EZB Electronic Journals Library</source><creator>Romano, Leonard E. C. ; Behrendt, Manuel ; Burkert, Andreas</creator><creatorcontrib>Romano, Leonard E. C. ; Behrendt, Manuel ; Burkert, Andreas</creatorcontrib><description>The deposition of energy and momentum by supernova explosions has been subject to numerous studies in the past few decades. However, while there has been some work that focused on the transition from the adiabatic to the radiative stage of a supernova remnant (SNR), the late radiative stage and merging with the interstellar medium (ISM) have received little attention. Here, we use three-dimensional, hydrodynamic simulations, focusing on the evolution of SNRs during the radiative phase, considering a wide range of physical explosion parameters (
n
H
,
ISM
∈
0.1
,
100
cm
−
3
and
E
SN
∈
1
,
14
×
10
51
erg
). We find that the radiative phase can be subdivided in four stages: A pressure-driven snowplow phase, during which the hot overpressurized bubble gas is evacuated and pushed into the cold shell; a momentum-conserving snowplow phase that is accompanied by a broadening of the shell; an implosion phase where cold material from the back of the shell is flooding the central vacuum; and a final cloud phase, during which the imploding gas is settling as a central, compact overdensity. The launching timescale for the implosion ranges from a few 100 kyr to a few Myr, while the cloud formation timescale ranges from a few to about 10 Myr. The highly chemically enriched clouds can become massive (
M
cl
∼ 10
3
–10
4
M
⊙
) and self-gravitating within a few Myr after their formation, providing an attractive, novel pathway for supernova-induced star and planet formation in the ISM.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ad2c05</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Cloud formation ; Dense interstellar clouds ; Explosions ; Gravitation ; Hydrodynamical simulations ; Implosions ; Interstellar dynamics ; Interstellar matter ; Interstellar medium ; Momentum ; Planet formation ; Shocks ; Supernova ; Supernova remnants ; Time</subject><ispartof>The Astrophysical journal, 2024-04, Vol.965 (2), p.168</ispartof><rights>2024. The Author(s). Published by the American Astronomical Society.</rights><rights>2024. The Author(s). Published by the American Astronomical Society. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><cites>FETCH-LOGICAL-c399t-f764046e76f0d5598f4e40802417731fec61af1b3519d3457f7eced3e4123a0f3</cites><orcidid>0000-0001-8404-3507 ; 0000-0002-8759-941X</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/ad2c05/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>315,781,785,865,2103,27929,27930,38895,53872</link.rule.ids></links><search><creatorcontrib>Romano, Leonard E. C.</creatorcontrib><creatorcontrib>Behrendt, Manuel</creatorcontrib><creatorcontrib>Burkert, Andreas</creatorcontrib><title>Cloud Formation by Supernova Implosion</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>The deposition of energy and momentum by supernova explosions has been subject to numerous studies in the past few decades. However, while there has been some work that focused on the transition from the adiabatic to the radiative stage of a supernova remnant (SNR), the late radiative stage and merging with the interstellar medium (ISM) have received little attention. Here, we use three-dimensional, hydrodynamic simulations, focusing on the evolution of SNRs during the radiative phase, considering a wide range of physical explosion parameters (
n
H
,
ISM
∈
0.1
,
100
cm
−
3
and
E
SN
∈
1
,
14
×
10
51
erg
). We find that the radiative phase can be subdivided in four stages: A pressure-driven snowplow phase, during which the hot overpressurized bubble gas is evacuated and pushed into the cold shell; a momentum-conserving snowplow phase that is accompanied by a broadening of the shell; an implosion phase where cold material from the back of the shell is flooding the central vacuum; and a final cloud phase, during which the imploding gas is settling as a central, compact overdensity. The launching timescale for the implosion ranges from a few 100 kyr to a few Myr, while the cloud formation timescale ranges from a few to about 10 Myr. The highly chemically enriched clouds can become massive (
M
cl
∼ 10
3
–10
4
M
⊙
) and self-gravitating within a few Myr after their formation, providing an attractive, novel pathway for supernova-induced star and planet formation in the ISM.</description><subject>Cloud formation</subject><subject>Dense interstellar clouds</subject><subject>Explosions</subject><subject>Gravitation</subject><subject>Hydrodynamical simulations</subject><subject>Implosions</subject><subject>Interstellar dynamics</subject><subject>Interstellar matter</subject><subject>Interstellar medium</subject><subject>Momentum</subject><subject>Planet formation</subject><subject>Shocks</subject><subject>Supernova</subject><subject>Supernova remnants</subject><subject>Time</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2024</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><sourceid>DOA</sourceid><recordid>eNp9kM1LxDAQxYMouK7ePRZET9adNN9HWVxdEDyo4C2kTSIt3U1NW2H_e1sr60U8DfN482bmh9A5hhsiqVhgRmRKCRMLY7MC2AGa7aVDNAMAmnIi3o7RSdtWY5spNUNXyzr0NlmFuDFdGbZJvkue-8bFbfg0yXrT1KEd5FN05E3durOfOkevq7uX5UP6-HS_Xt4-pgVRqku94BQod4J7sIwp6amjICGjWAiCvSs4Nh7nhGFlCWXCC1c4SxzFGTHgyRytp1wbTKWbWG5M3OlgSv0thPiuTezKonaac-ttQfNcQkGthVxiTwAL6a2zw-tD1sWU1cTw0bu201Xo43Y4XxOgwBRjIAcXTK4ihraNzu-3YtAjWT1i1CNGPZEdRq6nkTI0v5n_2C__sJum0ooznWnMpW6sJ1-NTIR-</recordid><startdate>20240401</startdate><enddate>20240401</enddate><creator>Romano, Leonard E. C.</creator><creator>Behrendt, Manuel</creator><creator>Burkert, Andreas</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>O3W</scope><scope>TSCCA</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>DOA</scope><orcidid>https://orcid.org/0000-0001-8404-3507</orcidid><orcidid>https://orcid.org/0000-0002-8759-941X</orcidid></search><sort><creationdate>20240401</creationdate><title>Cloud Formation by Supernova Implosion</title><author>Romano, Leonard E. C. ; Behrendt, Manuel ; Burkert, Andreas</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c399t-f764046e76f0d5598f4e40802417731fec61af1b3519d3457f7eced3e4123a0f3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2024</creationdate><topic>Cloud formation</topic><topic>Dense interstellar clouds</topic><topic>Explosions</topic><topic>Gravitation</topic><topic>Hydrodynamical simulations</topic><topic>Implosions</topic><topic>Interstellar dynamics</topic><topic>Interstellar matter</topic><topic>Interstellar medium</topic><topic>Momentum</topic><topic>Planet formation</topic><topic>Shocks</topic><topic>Supernova</topic><topic>Supernova remnants</topic><topic>Time</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Romano, Leonard E. C.</creatorcontrib><creatorcontrib>Behrendt, Manuel</creatorcontrib><creatorcontrib>Burkert, Andreas</creatorcontrib><collection>Open Access: IOP Publishing Free Content</collection><collection>IOPscience (Open Access)</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>DOAJ Directory of Open Access Journals</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Romano, Leonard E. C.</au><au>Behrendt, Manuel</au><au>Burkert, Andreas</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Cloud Formation by Supernova Implosion</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2024-04-01</date><risdate>2024</risdate><volume>965</volume><issue>2</issue><spage>168</spage><pages>168-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>The deposition of energy and momentum by supernova explosions has been subject to numerous studies in the past few decades. However, while there has been some work that focused on the transition from the adiabatic to the radiative stage of a supernova remnant (SNR), the late radiative stage and merging with the interstellar medium (ISM) have received little attention. Here, we use three-dimensional, hydrodynamic simulations, focusing on the evolution of SNRs during the radiative phase, considering a wide range of physical explosion parameters (
n
H
,
ISM
∈
0.1
,
100
cm
−
3
and
E
SN
∈
1
,
14
×
10
51
erg
). We find that the radiative phase can be subdivided in four stages: A pressure-driven snowplow phase, during which the hot overpressurized bubble gas is evacuated and pushed into the cold shell; a momentum-conserving snowplow phase that is accompanied by a broadening of the shell; an implosion phase where cold material from the back of the shell is flooding the central vacuum; and a final cloud phase, during which the imploding gas is settling as a central, compact overdensity. The launching timescale for the implosion ranges from a few 100 kyr to a few Myr, while the cloud formation timescale ranges from a few to about 10 Myr. The highly chemically enriched clouds can become massive (
M
cl
∼ 10
3
–10
4
M
⊙
) and self-gravitating within a few Myr after their formation, providing an attractive, novel pathway for supernova-induced star and planet formation in the ISM.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/ad2c05</doi><tpages>15</tpages><orcidid>https://orcid.org/0000-0001-8404-3507</orcidid><orcidid>https://orcid.org/0000-0002-8759-941X</orcidid><oa>free_for_read</oa></addata></record> |
fulltext | fulltext |
identifier | ISSN: 0004-637X |
ispartof | The Astrophysical journal, 2024-04, Vol.965 (2), p.168 |
issn | 0004-637X 1538-4357 |
language | eng |
recordid | cdi_crossref_primary_10_3847_1538_4357_ad2c05 |
source | Open Access: IOP Publishing Free Content; DOAJ Directory of Open Access Journals; Alma/SFX Local Collection; EZB Electronic Journals Library |
subjects | Cloud formation Dense interstellar clouds Explosions Gravitation Hydrodynamical simulations Implosions Interstellar dynamics Interstellar matter Interstellar medium Momentum Planet formation Shocks Supernova Supernova remnants Time |
title | Cloud Formation by Supernova Implosion |
url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-12-13T20%3A41%3A23IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_cross&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Cloud%20Formation%20by%20Supernova%20Implosion&rft.jtitle=The%20Astrophysical%20journal&rft.au=Romano,%20Leonard%20E.%20C.&rft.date=2024-04-01&rft.volume=965&rft.issue=2&rft.spage=168&rft.pages=168-&rft.issn=0004-637X&rft.eissn=1538-4357&rft_id=info:doi/10.3847/1538-4357/ad2c05&rft_dat=%3Cproquest_cross%3E3040595508%3C/proquest_cross%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=3040595508&rft_id=info:pmid/&rft_doaj_id=oai_doaj_org_article_66dfdc4bb80c4dd0b81f30178fded153&rfr_iscdi=true |