An Alternative Model for the Orbital Decay of M82 X-2: The Anomalous Magnetic Braking of a Bp Star
Recently, the first pulsating ultraluminous X-ray source M82 X-2 was reported to be experiencing a rapid orbital decay at a rate of P ̇ = − ( 5.69 ± 0.24 ) × 10 − 8 s s − 1 based on 7 yr NuSTAR data. To account for the observed orbital-period derivative, it requires a mass transfer rate of ∼ 200 M ̇...
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| Veröffentlicht in: | The Astrophysical journal 2024-09, Vol.973 (1), p.38 |
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| description | Recently, the first pulsating ultraluminous X-ray source M82 X-2 was reported to be experiencing a rapid orbital decay at a rate of
P
̇
=
−
(
5.69
±
0.24
)
×
10
−
8
s
s
−
1
based on 7 yr NuSTAR data. To account for the observed orbital-period derivative, it requires a mass transfer rate of
∼
200
M
̇
edd
(
M
̇
edd
is the Eddington accretion rate) from the donor star to the accreting neutron star. However, other potential models cannot be completely excluded. In this work, we propose an anomalous magnetic braking (AMB) model to interpret the detected orbital decay of M82 X-2. If the donor star is an Ap/Bp star with an anomalously strong magnetic field, the magnetic coupling between strong surface magnetic field and irradiation-driven wind from the surface of the donor star could cause an efficient angular-momentum loss, driving a rapid orbital decay observed in M82 X-2. The AMB mechanism of an Ap/Bp star with a mass of 5.0–15.0
M
⊙
and a surface magnetic field of 3000–4500 G could produce the observed
P
̇
of M82 X-2. We also discuss the possibility of other alternative models including the companion star expansion and a surrounding circumbinary disk. |
| doi_str_mv | 10.3847/1538-4357/ad66ce |
| format | Article |
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P
̇
=
−
(
5.69
±
0.24
)
×
10
−
8
s
s
−
1
based on 7 yr NuSTAR data. To account for the observed orbital-period derivative, it requires a mass transfer rate of
∼
200
M
̇
edd
(
M
̇
edd
is the Eddington accretion rate) from the donor star to the accreting neutron star. However, other potential models cannot be completely excluded. In this work, we propose an anomalous magnetic braking (AMB) model to interpret the detected orbital decay of M82 X-2. If the donor star is an Ap/Bp star with an anomalously strong magnetic field, the magnetic coupling between strong surface magnetic field and irradiation-driven wind from the surface of the donor star could cause an efficient angular-momentum loss, driving a rapid orbital decay observed in M82 X-2. The AMB mechanism of an Ap/Bp star with a mass of 5.0–15.0
M
⊙
and a surface magnetic field of 3000–4500 G could produce the observed
P
̇
of M82 X-2. We also discuss the possibility of other alternative models including the companion star expansion and a surrounding circumbinary disk.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ad66ce</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Accretion disks ; Angular momentum ; Binary stars ; Braking ; Companion stars ; Irradiation ; Magnetic fields ; Mass transfer ; Neutron stars ; Orbit decay ; Orbital evolution ; Stars ; Ultraluminous x-ray sources ; X ray sources ; X-ray binary stars</subject><ispartof>The Astrophysical journal, 2024-09, Vol.973 (1), p.38</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-c299t-fd95fe78c348e76882ba28a5fa85ff42d115d733c7df23d8abc35e2a856094ad3</cites><orcidid>0000-0002-0785-5349</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/ad66ce/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>314,776,780,860,2096,27901,27902,38867,53842</link.rule.ids></links><search><creatorcontrib>Chen, Wen-Cong</creatorcontrib><title>An Alternative Model for the Orbital Decay of M82 X-2: The Anomalous Magnetic Braking of a Bp Star</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>Recently, the first pulsating ultraluminous X-ray source M82 X-2 was reported to be experiencing a rapid orbital decay at a rate of
P
̇
=
−
(
5.69
±
0.24
)
×
10
−
8
s
s
−
1
based on 7 yr NuSTAR data. To account for the observed orbital-period derivative, it requires a mass transfer rate of
∼
200
M
̇
edd
(
M
̇
edd
is the Eddington accretion rate) from the donor star to the accreting neutron star. However, other potential models cannot be completely excluded. In this work, we propose an anomalous magnetic braking (AMB) model to interpret the detected orbital decay of M82 X-2. If the donor star is an Ap/Bp star with an anomalously strong magnetic field, the magnetic coupling between strong surface magnetic field and irradiation-driven wind from the surface of the donor star could cause an efficient angular-momentum loss, driving a rapid orbital decay observed in M82 X-2. The AMB mechanism of an Ap/Bp star with a mass of 5.0–15.0
M
⊙
and a surface magnetic field of 3000–4500 G could produce the observed
P
̇
of M82 X-2. We also discuss the possibility of other alternative models including the companion star expansion and a surrounding circumbinary disk.</description><subject>Accretion disks</subject><subject>Angular momentum</subject><subject>Binary stars</subject><subject>Braking</subject><subject>Companion stars</subject><subject>Irradiation</subject><subject>Magnetic fields</subject><subject>Mass transfer</subject><subject>Neutron stars</subject><subject>Orbit decay</subject><subject>Orbital evolution</subject><subject>Stars</subject><subject>Ultraluminous x-ray sources</subject><subject>X ray sources</subject><subject>X-ray binary stars</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>eNp1UctOwzAQtBBIlMedoyWuBBw_YptbeSNR9UCRuFkbP0pKiIuTIvH3JATBidNqZ2dmVzsIHeXklCkuz3LBVMaZkGfgisL6LTT5hbbRhBDCs4LJ512017aroaVaT1A5bfC07nxqoKs-PJ5F52scYsLdi8fzVFYd1PjKW_jEMeCZovg5o-d40U-nTXyDOm5aPINl47vK4osEr1WzHKiAL9b4sYN0gHYC1K0__Kn76OnmenF5lz3Mb-8vpw-Z7S_psuC0CF4qy7jyslCKlkAViABKhMCpy3PhJGNWukCZU1BaJjztpwXRHBzbR_ejr4uwMutUvUH6NBEq8w3EtDSQ-iNrb4gNpfRWK6os95wrylRpdaGlKwN1ovc6Hr3WKb5vfNuZVdz0P6pbw3IitNZcqp5FRpZNsW2TD79bc2KGVMwQgRkiMGMqveRklFRx_ef5L_0L7GeMEw</recordid><startdate>20240901</startdate><enddate>20240901</enddate><creator>Chen, Wen-Cong</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/0000-0002-0785-5349</orcidid></search><sort><creationdate>20240901</creationdate><title>An Alternative Model for the Orbital Decay of M82 X-2: The Anomalous Magnetic Braking of a Bp Star</title><author>Chen, Wen-Cong</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c299t-fd95fe78c348e76882ba28a5fa85ff42d115d733c7df23d8abc35e2a856094ad3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2024</creationdate><topic>Accretion disks</topic><topic>Angular momentum</topic><topic>Binary stars</topic><topic>Braking</topic><topic>Companion stars</topic><topic>Irradiation</topic><topic>Magnetic fields</topic><topic>Mass transfer</topic><topic>Neutron stars</topic><topic>Orbit decay</topic><topic>Orbital evolution</topic><topic>Stars</topic><topic>Ultraluminous x-ray sources</topic><topic>X ray sources</topic><topic>X-ray binary stars</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Chen, Wen-Cong</creatorcontrib><collection>IOP Publishing</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>Chen, Wen-Cong</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>An Alternative Model for the Orbital Decay of M82 X-2: The Anomalous Magnetic Braking of a Bp Star</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2024-09-01</date><risdate>2024</risdate><volume>973</volume><issue>1</issue><spage>38</spage><pages>38-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>Recently, the first pulsating ultraluminous X-ray source M82 X-2 was reported to be experiencing a rapid orbital decay at a rate of
P
̇
=
−
(
5.69
±
0.24
)
×
10
−
8
s
s
−
1
based on 7 yr NuSTAR data. To account for the observed orbital-period derivative, it requires a mass transfer rate of
∼
200
M
̇
edd
(
M
̇
edd
is the Eddington accretion rate) from the donor star to the accreting neutron star. However, other potential models cannot be completely excluded. In this work, we propose an anomalous magnetic braking (AMB) model to interpret the detected orbital decay of M82 X-2. If the donor star is an Ap/Bp star with an anomalously strong magnetic field, the magnetic coupling between strong surface magnetic field and irradiation-driven wind from the surface of the donor star could cause an efficient angular-momentum loss, driving a rapid orbital decay observed in M82 X-2. The AMB mechanism of an Ap/Bp star with a mass of 5.0–15.0
M
⊙
and a surface magnetic field of 3000–4500 G could produce the observed
P
̇
of M82 X-2. We also discuss the possibility of other alternative models including the companion star expansion and a surrounding circumbinary disk.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/ad66ce</doi><tpages>7</tpages><orcidid>https://orcid.org/0000-0002-0785-5349</orcidid><oa>free_for_read</oa></addata></record> |
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| source | DOAJ Directory of Open Access Journals; IOP Publishing; Alma/SFX Local Collection; EZB Electronic Journals Library |
| subjects | Accretion disks Angular momentum Binary stars Braking Companion stars Irradiation Magnetic fields Mass transfer Neutron stars Orbit decay Orbital evolution Stars Ultraluminous x-ray sources X ray sources X-ray binary stars |
| title | An Alternative Model for the Orbital Decay of M82 X-2: The Anomalous Magnetic Braking of a Bp Star |
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