An alternative evolution scenario for OAO 1657-415 and IGR J18483-0311
Abstract The relation between the spin period and the orbital period in high-mass X-ray binaries is investigated. Be/X-ray binaries and SG/X-ray binaries occupy different areas in Corbet’s diagram. The two SG/X-ray binaries, IGR J18483-0311 and OAO 1657-415, however, appear to occupy a transition re...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Liu, QingZhong [verfasserIn] Li, Hui [verfasserIn] Yan, JingZhi [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2010 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: Science in China - Heidelberg : Springer, 2003, 53(2010), Suppl 1 vom: Jan., Seite 130-134 |
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| Übergeordnetes Werk: |
volume:53 ; year:2010 ; number:Suppl 1 ; month:01 ; pages:130-134 |
| Links: |
|---|
| DOI / URN: |
10.1007/s11433-010-0005-5 |
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SPR019341717 |
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| 520 | |a Abstract The relation between the spin period and the orbital period in high-mass X-ray binaries is investigated. Be/X-ray binaries and SG/X-ray binaries occupy different areas in Corbet’s diagram. The two SG/X-ray binaries, IGR J18483-0311 and OAO 1657-415, however, appear to occupy a transition region between Be/X-ray binaries and wind-fed SG/X-ray binaries. This can be understood by noting that the neutron stars in the two SG/X-ray binaries have not reached their equilibrium spin periods when the donors evolved off the main sequence. Here, we provide an alternative scenario to explain their location in Corbet’s diagram: the SG/X-ray binaries are the descendants of Be/X-ray binaries, i.e. the supergiants in these systems were formed from O-type emission line stars instead of normal main-sequence stars. Furthermore, we suggest that there are two types of SG/X-ray binaries: one is directly evolved from a normal OB-type main sequence and neutron star system without an X-ray history, and the other evolved from a Be/X-ray binary with an X-ray history. | ||
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| 650 | 4 | |a stellar evolution |7 (dpeaa)DE-He213 | |
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10.1007/s11433-010-0005-5 doi (DE-627)SPR019341717 (SPR)s11433-010-0005-5-e DE-627 ger DE-627 rakwb eng 530 520 ASE 33.00 bkl 39.00 bkl Liu, QingZhong verfasserin aut An alternative evolution scenario for OAO 1657-415 and IGR J18483-0311 2010 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The relation between the spin period and the orbital period in high-mass X-ray binaries is investigated. Be/X-ray binaries and SG/X-ray binaries occupy different areas in Corbet’s diagram. The two SG/X-ray binaries, IGR J18483-0311 and OAO 1657-415, however, appear to occupy a transition region between Be/X-ray binaries and wind-fed SG/X-ray binaries. This can be understood by noting that the neutron stars in the two SG/X-ray binaries have not reached their equilibrium spin periods when the donors evolved off the main sequence. Here, we provide an alternative scenario to explain their location in Corbet’s diagram: the SG/X-ray binaries are the descendants of Be/X-ray binaries, i.e. the supergiants in these systems were formed from O-type emission line stars instead of normal main-sequence stars. Furthermore, we suggest that there are two types of SG/X-ray binaries: one is directly evolved from a normal OB-type main sequence and neutron star system without an X-ray history, and the other evolved from a Be/X-ray binary with an X-ray history. high-mass X-ray binary (dpeaa)DE-He213 pulsar (dpeaa)DE-He213 Corbet’s diagram (dpeaa)DE-He213 stellar evolution (dpeaa)DE-He213 Li, Hui verfasserin aut Yan, JingZhi verfasserin aut Enthalten in Science in China Heidelberg : Springer, 2003 53(2010), Suppl 1 vom: Jan., Seite 130-134 (DE-627)385614799 (DE-600)2142901-7 1862-2844 nnns volume:53 year:2010 number:Suppl 1 month:01 pages:130-134 https://dx.doi.org/10.1007/s11433-010-0005-5 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_152 GBV_ILN_161 GBV_ILN_171 GBV_ILN_187 GBV_ILN_224 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 33.00 ASE 39.00 ASE AR 53 2010 Suppl 1 01 130-134 |
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10.1007/s11433-010-0005-5 doi (DE-627)SPR019341717 (SPR)s11433-010-0005-5-e DE-627 ger DE-627 rakwb eng 530 520 ASE 33.00 bkl 39.00 bkl Liu, QingZhong verfasserin aut An alternative evolution scenario for OAO 1657-415 and IGR J18483-0311 2010 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The relation between the spin period and the orbital period in high-mass X-ray binaries is investigated. Be/X-ray binaries and SG/X-ray binaries occupy different areas in Corbet’s diagram. The two SG/X-ray binaries, IGR J18483-0311 and OAO 1657-415, however, appear to occupy a transition region between Be/X-ray binaries and wind-fed SG/X-ray binaries. This can be understood by noting that the neutron stars in the two SG/X-ray binaries have not reached their equilibrium spin periods when the donors evolved off the main sequence. Here, we provide an alternative scenario to explain their location in Corbet’s diagram: the SG/X-ray binaries are the descendants of Be/X-ray binaries, i.e. the supergiants in these systems were formed from O-type emission line stars instead of normal main-sequence stars. Furthermore, we suggest that there are two types of SG/X-ray binaries: one is directly evolved from a normal OB-type main sequence and neutron star system without an X-ray history, and the other evolved from a Be/X-ray binary with an X-ray history. high-mass X-ray binary (dpeaa)DE-He213 pulsar (dpeaa)DE-He213 Corbet’s diagram (dpeaa)DE-He213 stellar evolution (dpeaa)DE-He213 Li, Hui verfasserin aut Yan, JingZhi verfasserin aut Enthalten in Science in China Heidelberg : Springer, 2003 53(2010), Suppl 1 vom: Jan., Seite 130-134 (DE-627)385614799 (DE-600)2142901-7 1862-2844 nnns volume:53 year:2010 number:Suppl 1 month:01 pages:130-134 https://dx.doi.org/10.1007/s11433-010-0005-5 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_152 GBV_ILN_161 GBV_ILN_171 GBV_ILN_187 GBV_ILN_224 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 33.00 ASE 39.00 ASE AR 53 2010 Suppl 1 01 130-134 |
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10.1007/s11433-010-0005-5 doi (DE-627)SPR019341717 (SPR)s11433-010-0005-5-e DE-627 ger DE-627 rakwb eng 530 520 ASE 33.00 bkl 39.00 bkl Liu, QingZhong verfasserin aut An alternative evolution scenario for OAO 1657-415 and IGR J18483-0311 2010 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The relation between the spin period and the orbital period in high-mass X-ray binaries is investigated. Be/X-ray binaries and SG/X-ray binaries occupy different areas in Corbet’s diagram. The two SG/X-ray binaries, IGR J18483-0311 and OAO 1657-415, however, appear to occupy a transition region between Be/X-ray binaries and wind-fed SG/X-ray binaries. This can be understood by noting that the neutron stars in the two SG/X-ray binaries have not reached their equilibrium spin periods when the donors evolved off the main sequence. Here, we provide an alternative scenario to explain their location in Corbet’s diagram: the SG/X-ray binaries are the descendants of Be/X-ray binaries, i.e. the supergiants in these systems were formed from O-type emission line stars instead of normal main-sequence stars. Furthermore, we suggest that there are two types of SG/X-ray binaries: one is directly evolved from a normal OB-type main sequence and neutron star system without an X-ray history, and the other evolved from a Be/X-ray binary with an X-ray history. high-mass X-ray binary (dpeaa)DE-He213 pulsar (dpeaa)DE-He213 Corbet’s diagram (dpeaa)DE-He213 stellar evolution (dpeaa)DE-He213 Li, Hui verfasserin aut Yan, JingZhi verfasserin aut Enthalten in Science in China Heidelberg : Springer, 2003 53(2010), Suppl 1 vom: Jan., Seite 130-134 (DE-627)385614799 (DE-600)2142901-7 1862-2844 nnns volume:53 year:2010 number:Suppl 1 month:01 pages:130-134 https://dx.doi.org/10.1007/s11433-010-0005-5 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_152 GBV_ILN_161 GBV_ILN_171 GBV_ILN_187 GBV_ILN_224 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 33.00 ASE 39.00 ASE AR 53 2010 Suppl 1 01 130-134 |
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10.1007/s11433-010-0005-5 doi (DE-627)SPR019341717 (SPR)s11433-010-0005-5-e DE-627 ger DE-627 rakwb eng 530 520 ASE 33.00 bkl 39.00 bkl Liu, QingZhong verfasserin aut An alternative evolution scenario for OAO 1657-415 and IGR J18483-0311 2010 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The relation between the spin period and the orbital period in high-mass X-ray binaries is investigated. Be/X-ray binaries and SG/X-ray binaries occupy different areas in Corbet’s diagram. The two SG/X-ray binaries, IGR J18483-0311 and OAO 1657-415, however, appear to occupy a transition region between Be/X-ray binaries and wind-fed SG/X-ray binaries. This can be understood by noting that the neutron stars in the two SG/X-ray binaries have not reached their equilibrium spin periods when the donors evolved off the main sequence. Here, we provide an alternative scenario to explain their location in Corbet’s diagram: the SG/X-ray binaries are the descendants of Be/X-ray binaries, i.e. the supergiants in these systems were formed from O-type emission line stars instead of normal main-sequence stars. Furthermore, we suggest that there are two types of SG/X-ray binaries: one is directly evolved from a normal OB-type main sequence and neutron star system without an X-ray history, and the other evolved from a Be/X-ray binary with an X-ray history. high-mass X-ray binary (dpeaa)DE-He213 pulsar (dpeaa)DE-He213 Corbet’s diagram (dpeaa)DE-He213 stellar evolution (dpeaa)DE-He213 Li, Hui verfasserin aut Yan, JingZhi verfasserin aut Enthalten in Science in China Heidelberg : Springer, 2003 53(2010), Suppl 1 vom: Jan., Seite 130-134 (DE-627)385614799 (DE-600)2142901-7 1862-2844 nnns volume:53 year:2010 number:Suppl 1 month:01 pages:130-134 https://dx.doi.org/10.1007/s11433-010-0005-5 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_152 GBV_ILN_161 GBV_ILN_171 GBV_ILN_187 GBV_ILN_224 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 33.00 ASE 39.00 ASE AR 53 2010 Suppl 1 01 130-134 |
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10.1007/s11433-010-0005-5 doi (DE-627)SPR019341717 (SPR)s11433-010-0005-5-e DE-627 ger DE-627 rakwb eng 530 520 ASE 33.00 bkl 39.00 bkl Liu, QingZhong verfasserin aut An alternative evolution scenario for OAO 1657-415 and IGR J18483-0311 2010 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The relation between the spin period and the orbital period in high-mass X-ray binaries is investigated. Be/X-ray binaries and SG/X-ray binaries occupy different areas in Corbet’s diagram. The two SG/X-ray binaries, IGR J18483-0311 and OAO 1657-415, however, appear to occupy a transition region between Be/X-ray binaries and wind-fed SG/X-ray binaries. This can be understood by noting that the neutron stars in the two SG/X-ray binaries have not reached their equilibrium spin periods when the donors evolved off the main sequence. Here, we provide an alternative scenario to explain their location in Corbet’s diagram: the SG/X-ray binaries are the descendants of Be/X-ray binaries, i.e. the supergiants in these systems were formed from O-type emission line stars instead of normal main-sequence stars. Furthermore, we suggest that there are two types of SG/X-ray binaries: one is directly evolved from a normal OB-type main sequence and neutron star system without an X-ray history, and the other evolved from a Be/X-ray binary with an X-ray history. high-mass X-ray binary (dpeaa)DE-He213 pulsar (dpeaa)DE-He213 Corbet’s diagram (dpeaa)DE-He213 stellar evolution (dpeaa)DE-He213 Li, Hui verfasserin aut Yan, JingZhi verfasserin aut Enthalten in Science in China Heidelberg : Springer, 2003 53(2010), Suppl 1 vom: Jan., Seite 130-134 (DE-627)385614799 (DE-600)2142901-7 1862-2844 nnns volume:53 year:2010 number:Suppl 1 month:01 pages:130-134 https://dx.doi.org/10.1007/s11433-010-0005-5 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_152 GBV_ILN_161 GBV_ILN_171 GBV_ILN_187 GBV_ILN_224 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 33.00 ASE 39.00 ASE AR 53 2010 Suppl 1 01 130-134 |
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Be/X-ray binaries and SG/X-ray binaries occupy different areas in Corbet’s diagram. The two SG/X-ray binaries, IGR J18483-0311 and OAO 1657-415, however, appear to occupy a transition region between Be/X-ray binaries and wind-fed SG/X-ray binaries. This can be understood by noting that the neutron stars in the two SG/X-ray binaries have not reached their equilibrium spin periods when the donors evolved off the main sequence. Here, we provide an alternative scenario to explain their location in Corbet’s diagram: the SG/X-ray binaries are the descendants of Be/X-ray binaries, i.e. the supergiants in these systems were formed from O-type emission line stars instead of normal main-sequence stars. 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Abstract The relation between the spin period and the orbital period in high-mass X-ray binaries is investigated. Be/X-ray binaries and SG/X-ray binaries occupy different areas in Corbet’s diagram. The two SG/X-ray binaries, IGR J18483-0311 and OAO 1657-415, however, appear to occupy a transition region between Be/X-ray binaries and wind-fed SG/X-ray binaries. This can be understood by noting that the neutron stars in the two SG/X-ray binaries have not reached their equilibrium spin periods when the donors evolved off the main sequence. Here, we provide an alternative scenario to explain their location in Corbet’s diagram: the SG/X-ray binaries are the descendants of Be/X-ray binaries, i.e. the supergiants in these systems were formed from O-type emission line stars instead of normal main-sequence stars. Furthermore, we suggest that there are two types of SG/X-ray binaries: one is directly evolved from a normal OB-type main sequence and neutron star system without an X-ray history, and the other evolved from a Be/X-ray binary with an X-ray history. |
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Abstract The relation between the spin period and the orbital period in high-mass X-ray binaries is investigated. Be/X-ray binaries and SG/X-ray binaries occupy different areas in Corbet’s diagram. The two SG/X-ray binaries, IGR J18483-0311 and OAO 1657-415, however, appear to occupy a transition region between Be/X-ray binaries and wind-fed SG/X-ray binaries. This can be understood by noting that the neutron stars in the two SG/X-ray binaries have not reached their equilibrium spin periods when the donors evolved off the main sequence. Here, we provide an alternative scenario to explain their location in Corbet’s diagram: the SG/X-ray binaries are the descendants of Be/X-ray binaries, i.e. the supergiants in these systems were formed from O-type emission line stars instead of normal main-sequence stars. Furthermore, we suggest that there are two types of SG/X-ray binaries: one is directly evolved from a normal OB-type main sequence and neutron star system without an X-ray history, and the other evolved from a Be/X-ray binary with an X-ray history. |
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Abstract The relation between the spin period and the orbital period in high-mass X-ray binaries is investigated. Be/X-ray binaries and SG/X-ray binaries occupy different areas in Corbet’s diagram. The two SG/X-ray binaries, IGR J18483-0311 and OAO 1657-415, however, appear to occupy a transition region between Be/X-ray binaries and wind-fed SG/X-ray binaries. This can be understood by noting that the neutron stars in the two SG/X-ray binaries have not reached their equilibrium spin periods when the donors evolved off the main sequence. Here, we provide an alternative scenario to explain their location in Corbet’s diagram: the SG/X-ray binaries are the descendants of Be/X-ray binaries, i.e. the supergiants in these systems were formed from O-type emission line stars instead of normal main-sequence stars. Furthermore, we suggest that there are two types of SG/X-ray binaries: one is directly evolved from a normal OB-type main sequence and neutron star system without an X-ray history, and the other evolved from a Be/X-ray binary with an X-ray history. |
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