A Gaia view of the optical and X-ray luminosities of compact binary millisecond pulsars
In this paper, we study compact binary millisecond pulsars with low- and very low-mass companion stars (spiders) in the Galactic field, using data from the latest Gaia data release (DR3). We infer the parallax distances of the optical counterparts to spiders, which we use to estimate optical and X-r...
| Autores: | , |
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| Formato: | artículo |
| Fecha de publicación: | 2023 |
| País: | España |
| Recursos: | Universitat Politècnica de Catalunya (UPC) |
| Repositorio: | UPCommons. Portal del coneixement obert de la UPC |
| Idioma: | inglés |
| OAI Identifier: | oai:upcommons.upc.edu:2117/396210 |
| Acesso em linha: | https://hdl.handle.net/2117/396210 https://dx.doi.org/10.1093/mnras/stad2485 |
| Access Level: | acceso abierto |
| Palavra-chave: | Pulsars Neutron stars X-ray binaries Stars distances Neutron X-rays: binaries. Púlsars Estels de neutrons Estels binaris de raigs X Àrees temàtiques de la UPC::Física::Astronomia i astrofísica |
| Resumo: | In this paper, we study compact binary millisecond pulsars with low- and very low-mass companion stars (spiders) in the Galactic field, using data from the latest Gaia data release (DR3). We infer the parallax distances of the optical counterparts to spiders, which we use to estimate optical and X-ray luminosities. We compare the parallax distances to those derived from radio pulse dispersion measures and find that they have systematically larger values, by 40 per cent on average. We also test the correlation between X-ray and spin-down luminosities, finding that most redbacks have a spin-down to X-ray luminosity conversion efficiency of ~0.1 per cent, indicating a contribution from the intrabinary shock. On the other hand, most black widows have an efficiency of ~0.01 per cent, similar to the majority of the pulsar population. Finally, we find that the bolometric optical luminosity significantly correlates with the orbital period, with a large scatter due to different irradiated stellar temperatures and binary properties. We interpret this correlation as the effect of the increasing size of the Roche Lobe radius with the orbital period. With this newly found correlation, an estimate of the optical magnitude can be obtained from the orbital period and a distance estimate. |
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