The progenitor of binary millisecond radio pulsar PSR J1713+0747
- Autores
- Chen, W. C.; Panei, Jorge Alejandro
- Año de publicación
- 2011
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Context. PSR J1713+0747 is a binary system comprising millisecond radio pulsar with a spin period of 4.57 ms, and a low-mass white dwarf (WD) companion orbiting the pulsar with a period of 67.8 days. Using the general relativistic Shapiro delay, the masses of the WD and pulsar components were previously found to be 0.28 ± 0.03 M⊙ and 1.3 ± 0.2 M ⊙ (68% confidence), respectively. Aims. Standard binary evolution theory suggests that PSR J1713+0747 evolved from a low-mass X-ray binary (LMXB). Here, we test this hypothesis. Methods. We used a binary evolution code and a WD evolution code to calculate evolutionary sequences of LMXBs that could result in binary millisecond radio pulsars such as PSR J1713+0747. Results. During the mass exchange, the mass transfer is nonconservative. Because of the thermal and viscous instabilities developing in the accretion disk, the neutron star accretes only a small part of the incoming material. We find that the progenitor of PSR J1713+0747 can be modelled as an LMXB including a donor star with mass 1.3 - 1.6 M⊙ and an initial orbital period ranging from 2.40 to 4.15 days. If the cooling timescale of the WD is 8 Gyr, its present effective temperature is between 3870 and 4120 K, slightly higher than the observed value. We estimate a surface gravity of Log(g) ≈ 7.38 - 7.40.
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Ciencias Astronómicas
pulsars: general
stars: low-mass
white dwarfs
Estrellas - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/84271
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The progenitor of binary millisecond radio pulsar PSR J1713+0747Chen, W. C.Panei, Jorge AlejandroCiencias Astronómicaspulsars: generalstars: low-masswhite dwarfsEstrellas<b>Context.</b> PSR J1713+0747 is a binary system comprising millisecond radio pulsar with a spin period of 4.57 ms, and a low-mass white dwarf (WD) companion orbiting the pulsar with a period of 67.8 days. Using the general relativistic Shapiro delay, the masses of the WD and pulsar components were previously found to be 0.28 ± 0.03 M⊙ and 1.3 ± 0.2 M ⊙ (68% confidence), respectively. <b>Aims.</b> Standard binary evolution theory suggests that PSR J1713+0747 evolved from a low-mass X-ray binary (LMXB). Here, we test this hypothesis. <b>Methods.</b> We used a binary evolution code and a WD evolution code to calculate evolutionary sequences of LMXBs that could result in binary millisecond radio pulsars such as PSR J1713+0747. <b>Results.</b> During the mass exchange, the mass transfer is nonconservative. Because of the thermal and viscous instabilities developing in the accretion disk, the neutron star accretes only a small part of the incoming material. We find that the progenitor of PSR J1713+0747 can be modelled as an LMXB including a donor star with mass 1.3 - 1.6 M⊙ and an initial orbital period ranging from 2.40 to 4.15 days. If the cooling timescale of the WD is 8 Gyr, its present effective temperature is between 3870 and 4120 K, slightly higher than the observed value. We estimate a surface gravity of Log(g) ≈ 7.38 - 7.40.Facultad de Ciencias Astronómicas y Geofísicas2011-03info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/84271enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201014833info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:16:10Zoai:sedici.unlp.edu.ar:10915/84271Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:10.338SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
The progenitor of binary millisecond radio pulsar PSR J1713+0747 |
title |
The progenitor of binary millisecond radio pulsar PSR J1713+0747 |
spellingShingle |
The progenitor of binary millisecond radio pulsar PSR J1713+0747 Chen, W. C. Ciencias Astronómicas pulsars: general stars: low-mass white dwarfs Estrellas |
title_short |
The progenitor of binary millisecond radio pulsar PSR J1713+0747 |
title_full |
The progenitor of binary millisecond radio pulsar PSR J1713+0747 |
title_fullStr |
The progenitor of binary millisecond radio pulsar PSR J1713+0747 |
title_full_unstemmed |
The progenitor of binary millisecond radio pulsar PSR J1713+0747 |
title_sort |
The progenitor of binary millisecond radio pulsar PSR J1713+0747 |
dc.creator.none.fl_str_mv |
Chen, W. C. Panei, Jorge Alejandro |
author |
Chen, W. C. |
author_facet |
Chen, W. C. Panei, Jorge Alejandro |
author_role |
author |
author2 |
Panei, Jorge Alejandro |
author2_role |
author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas pulsars: general stars: low-mass white dwarfs Estrellas |
topic |
Ciencias Astronómicas pulsars: general stars: low-mass white dwarfs Estrellas |
dc.description.none.fl_txt_mv |
<b>Context.</b> PSR J1713+0747 is a binary system comprising millisecond radio pulsar with a spin period of 4.57 ms, and a low-mass white dwarf (WD) companion orbiting the pulsar with a period of 67.8 days. Using the general relativistic Shapiro delay, the masses of the WD and pulsar components were previously found to be 0.28 ± 0.03 M⊙ and 1.3 ± 0.2 M ⊙ (68% confidence), respectively. <b>Aims.</b> Standard binary evolution theory suggests that PSR J1713+0747 evolved from a low-mass X-ray binary (LMXB). Here, we test this hypothesis. <b>Methods.</b> We used a binary evolution code and a WD evolution code to calculate evolutionary sequences of LMXBs that could result in binary millisecond radio pulsars such as PSR J1713+0747. <b>Results.</b> During the mass exchange, the mass transfer is nonconservative. Because of the thermal and viscous instabilities developing in the accretion disk, the neutron star accretes only a small part of the incoming material. We find that the progenitor of PSR J1713+0747 can be modelled as an LMXB including a donor star with mass 1.3 - 1.6 M⊙ and an initial orbital period ranging from 2.40 to 4.15 days. If the cooling timescale of the WD is 8 Gyr, its present effective temperature is between 3870 and 4120 K, slightly higher than the observed value. We estimate a surface gravity of Log(g) ≈ 7.38 - 7.40. Facultad de Ciencias Astronómicas y Geofísicas |
description |
<b>Context.</b> PSR J1713+0747 is a binary system comprising millisecond radio pulsar with a spin period of 4.57 ms, and a low-mass white dwarf (WD) companion orbiting the pulsar with a period of 67.8 days. Using the general relativistic Shapiro delay, the masses of the WD and pulsar components were previously found to be 0.28 ± 0.03 M⊙ and 1.3 ± 0.2 M ⊙ (68% confidence), respectively. <b>Aims.</b> Standard binary evolution theory suggests that PSR J1713+0747 evolved from a low-mass X-ray binary (LMXB). Here, we test this hypothesis. <b>Methods.</b> We used a binary evolution code and a WD evolution code to calculate evolutionary sequences of LMXBs that could result in binary millisecond radio pulsars such as PSR J1713+0747. <b>Results.</b> During the mass exchange, the mass transfer is nonconservative. Because of the thermal and viscous instabilities developing in the accretion disk, the neutron star accretes only a small part of the incoming material. We find that the progenitor of PSR J1713+0747 can be modelled as an LMXB including a donor star with mass 1.3 - 1.6 M⊙ and an initial orbital period ranging from 2.40 to 4.15 days. If the cooling timescale of the WD is 8 Gyr, its present effective temperature is between 3870 and 4120 K, slightly higher than the observed value. We estimate a surface gravity of Log(g) ≈ 7.38 - 7.40. |
publishDate |
2011 |
dc.date.none.fl_str_mv |
2011-03 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion Articulo http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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article |
status_str |
publishedVersion |
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http://sedici.unlp.edu.ar/handle/10915/84271 |
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http://sedici.unlp.edu.ar/handle/10915/84271 |
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eng |
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eng |
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info:eu-repo/semantics/altIdentifier/issn/0004-6361 info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201014833 |
dc.rights.none.fl_str_mv |
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