Relativistic effects in a mildly recycled pulsar binary: PSR J1952+2630
We report the results of timing observations of PSR J1952+2630, a 20.7 ms pulsar in orbit with a massive white dwarf companion. We performed six months of timing observations with the Arecibo radio telescope in 2020 and used data from FAST from 2021. Together with previously published data, this rep...
| Autores: | , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2022 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/295654 |
| Acceso en línea: | http://hdl.handle.net/10261/295654 |
| Access Level: | acceso abierto |
| Palabra clave: | Binaries: close Pulsars: individual: J1952+2630 Relativistic processes Stars: neutron Dense matter |
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| dc.title.none.fl_str_mv |
Relativistic effects in a mildly recycled pulsar binary: PSR J1952+2630 |
| title |
Relativistic effects in a mildly recycled pulsar binary: PSR J1952+2630 |
| spellingShingle |
Relativistic effects in a mildly recycled pulsar binary: PSR J1952+2630 Gautam, T. Binaries: close Pulsars: individual: J1952+2630 Relativistic processes Stars: neutron Dense matter |
| title_short |
Relativistic effects in a mildly recycled pulsar binary: PSR J1952+2630 |
| title_full |
Relativistic effects in a mildly recycled pulsar binary: PSR J1952+2630 |
| title_fullStr |
Relativistic effects in a mildly recycled pulsar binary: PSR J1952+2630 |
| title_full_unstemmed |
Relativistic effects in a mildly recycled pulsar binary: PSR J1952+2630 |
| title_sort |
Relativistic effects in a mildly recycled pulsar binary: PSR J1952+2630 |
| dc.creator.none.fl_str_mv |
Gautam, T. Freire, Paulo C. C. Batrakov, A. Kramer, Michael Miao, C. C. Parent, Emilie Zhu, W. W. |
| author |
Gautam, T. |
| author_facet |
Gautam, T. Freire, Paulo C. C. Batrakov, A. Kramer, Michael Miao, C. C. Parent, Emilie Zhu, W. W. |
| author_role |
author |
| author2 |
Freire, Paulo C. C. Batrakov, A. Kramer, Michael Miao, C. C. Parent, Emilie Zhu, W. W. |
| author2_role |
author author author author author author |
| dc.contributor.none.fl_str_mv |
Chinese Academy of Sciences European Research Council European Commission Agencia Estatal de Investigación (España) Ministerio de Ciencia, Innovación y Universidades (España) Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72] |
| dc.subject.none.fl_str_mv |
Binaries: close Pulsars: individual: J1952+2630 Relativistic processes Stars: neutron Dense matter |
| topic |
Binaries: close Pulsars: individual: J1952+2630 Relativistic processes Stars: neutron Dense matter |
| description |
We report the results of timing observations of PSR J1952+2630, a 20.7 ms pulsar in orbit with a massive white dwarf companion. We performed six months of timing observations with the Arecibo radio telescope in 2020 and used data from FAST from 2021. Together with previously published data, this represents a total timing baseline of 11 yr since the discovery of the pulsar in 2010. For the first time, we present a polarimetric profile of the pulsar and determine its rotation measure (RM), − 145.79 ± 0.15 rad m−2. With the increased timing baseline, we obtain improved estimates for astrometric, spin, and binary parameters for this system. In particular, we obtain an imporvement of an order of magnitude on the proper motion, and, for the first time, we detect three post-Keplerian parameters in this system: the advance of periastron ω̇, the orbital decay Ṗb, and the Shapiro delay (measured in the form of the h3 parameter). With the detection of these relativistic effects, we constrain the pulsar mass to 1.20−0.29+0.28 M⊙ and the mass of its companion to 0.97−0.13+0.16 M⊙. The current value of Ṗb is consistent with the General Relativity expectation for the masses obtained using ω̇ and h3. The excess (4.2−73.1+70.2 fs s−1) represents a limit on the emission of dipolar gravitational waves (GWs) from this system. This results in a limit on the difference in effective scalar couplings for the pulsar and companion (predicted by scalar-tensor theories of gravity; STTs) of |αp − αc|< 4.8 × 10−3 (68% C.L.), which does not yield a competitive test for STTs. However, our simulations of future timing campaigns of this system, based on the timing precision we have achieved with FAST, show that by 2032, the precision of Ṗb and ω̇ will allow for much more precise masses and much tighter constraints on the orbital decay contribution from dipolar GWs, resulting in |αp − αc|< 1.3 × 10−3 (68% C.L.). For comparison, we obtain |αp − αc|< 1.9 × 10−3 and < 3.3 × 10−3 from PSR J1738+0333 and PSR J2222−0137, respectively. We also present the constraints this system will place on the {α0, β0} parameters of Damour-Esposito-Farèse (DEF) gravity by 2032. They are comparable to those of PSR J1738+0333. Unlike PSR J1738+0333, PSR J1952+2630 will not be limited in its mass measurement and has the potential to place even more restrictive limits on DEF gravity in the future. Further improvements to this test will likely be limited by uncertainties in the kinematic contributions to Ṗb because of the lack of precise distance measurements. |
| publishDate |
2022 |
| dc.date.none.fl_str_mv |
2022 2023 2023 |
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info:eu-repo/semantics/article http://purl.org/coar/resource_type/c_6501 Publisher's version info:eu-repo/semantics/publishedVersion |
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article |
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http://hdl.handle.net/10261/295654 |
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http://hdl.handle.net/10261/295654 |
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Inglés |
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Inglés |
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Relativistic effects in a mildly recycled pulsar binary: PSR J1952+2630Gautam, T.Freire, Paulo C. C.Batrakov, A.Kramer, MichaelMiao, C. C.Parent, EmilieZhu, W. W.Binaries: closePulsars: individual: J1952+2630Relativistic processesStars: neutronDense matterWe report the results of timing observations of PSR J1952+2630, a 20.7 ms pulsar in orbit with a massive white dwarf companion. We performed six months of timing observations with the Arecibo radio telescope in 2020 and used data from FAST from 2021. Together with previously published data, this represents a total timing baseline of 11 yr since the discovery of the pulsar in 2010. For the first time, we present a polarimetric profile of the pulsar and determine its rotation measure (RM), − 145.79 ± 0.15 rad m−2. With the increased timing baseline, we obtain improved estimates for astrometric, spin, and binary parameters for this system. In particular, we obtain an imporvement of an order of magnitude on the proper motion, and, for the first time, we detect three post-Keplerian parameters in this system: the advance of periastron ω̇, the orbital decay Ṗb, and the Shapiro delay (measured in the form of the h3 parameter). With the detection of these relativistic effects, we constrain the pulsar mass to 1.20−0.29+0.28 M⊙ and the mass of its companion to 0.97−0.13+0.16 M⊙. The current value of Ṗb is consistent with the General Relativity expectation for the masses obtained using ω̇ and h3. The excess (4.2−73.1+70.2 fs s−1) represents a limit on the emission of dipolar gravitational waves (GWs) from this system. This results in a limit on the difference in effective scalar couplings for the pulsar and companion (predicted by scalar-tensor theories of gravity; STTs) of |αp − αc|< 4.8 × 10−3 (68% C.L.), which does not yield a competitive test for STTs. However, our simulations of future timing campaigns of this system, based on the timing precision we have achieved with FAST, show that by 2032, the precision of Ṗb and ω̇ will allow for much more precise masses and much tighter constraints on the orbital decay contribution from dipolar GWs, resulting in |αp − αc|< 1.3 × 10−3 (68% C.L.). For comparison, we obtain |αp − αc|< 1.9 × 10−3 and < 3.3 × 10−3 from PSR J1738+0333 and PSR J2222−0137, respectively. We also present the constraints this system will place on the {α0, β0} parameters of Damour-Esposito-Farèse (DEF) gravity by 2032. They are comparable to those of PSR J1738+0333. Unlike PSR J1738+0333, PSR J1952+2630 will not be limited in its mass measurement and has the potential to place even more restrictive limits on DEF gravity in the future. Further improvements to this test will likely be limited by uncertainties in the kinematic contributions to Ṗb because of the lack of precise distance measurements.This work made use of the data from FAST (Five-hundred-meter Aperture Spherical radio Telescope). FAST is a Chinese national mega-science facility, operated by National Astronomical Observatories, Chinese Academy of Sciences. EP supported by the H2020 ERC Consolidator Grant “MAGNESIA” under grant agreement No. 817661 and National Spanish grant PGC2018-095512-BI00.Peer reviewedEDP SciencesChinese Academy of SciencesEuropean Research CouncilEuropean CommissionAgencia Estatal de Investigación (España)Ministerio de Ciencia, Innovación y Universidades (España)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202320232022info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/295654reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PGC2018-095512-B-I00info:eu-repo/grantAgreement/EC/H2020/817661Astronomy and Astrophysicshttps://doi.org/10.1051/0004-6361/202244699Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2956542026-05-22T06:33:51Z |
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