Synthetic X-ray emission from white dwarf accreting planetary material


Por: Estrada-Dorado S., Lora V., Toalá J.A., Esquivel A., Guerrero M.A., Maldonado R.F., Chu Y.-H.

Publicada: 1 ene 2024
Resumen:
The emission of hard X-rays associated with white dwarfs (WDs) can be generated by the presence of a stellar companion, either by the companion's coronal emission or by an accretion disc formed by the material stripped from the companion. Recent studies have suggested that a Jupiter-like planet can also be a donor of the material whose accretion on to the WD can generate hard X-rays. We use the guacho code to reproduce the conditions of this WD-planet scenario. With the example of the hard X-ray WD KPD 0005+5106, we explore different terminal wind velocities and mass-loss rates of a donor planet for a future network of simulations to investigate the luminosity and the spectral and temporal properties of the hard X-ray emission in the WD-planet systems. Our simulations show that the material stripped from the planet forms a disc and accretes on to the WD to reach temperatures high enough to generate hard X-rays as usually seen in X-ray binaries with low-mass companions. For high terminal wind velocities, the planet material does not form a disc, but it rather accretes directly on to the WD surface. The simulations reproduce the X-ray luminosity of another X-ray accreting WD (G 29-38), and only sometimes reaches the hard X-ray luminosity of KPD 0005+5106. The X-ray variability is stochastic and does not reproduce the period of KPD 0005+5106, suggesting that the additional physical processes (e.g. hot spots resulting from magnetic channelling of the accreting material) need to be explored. © 2023 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.

Filiaciones:
Estrada-Dorado S.:
 Instituto de Radioastronomía y Astrofísica, UNAM, Antigua Carretera A Pátzcuaro, 8701, Ex-Hda. San Jose de la Huerta, Mich, Morelia, 58089, Mexico

Lora V.:
 Instituto de Radioastronomía y Astrofísica, UNAM, Antigua Carretera A Pátzcuaro, 8701, Ex-Hda. San Jose de la Huerta, Mich, Morelia, 58089, Mexico

 Instituto de Ciencias Nucleares, UNAM, Apartado postal 73-543, Ciudad de México, 04510, Mexico

Toalá J.A.:
 Instituto de Radioastronomía y Astrofísica, UNAM, Antigua Carretera A Pátzcuaro, 8701, Ex-Hda. San Jose de la Huerta, Mich, Morelia, 58089, Mexico

Esquivel A.:
 Instituto de Ciencias Nucleares, UNAM, Apartado postal 73-543, Ciudad de México, 04510, Mexico

Guerrero M.A.:
 Instituto de Astrofísica de Andaluciá, CSIC, Glorieta de la Astronomiá s/n, Granada, E-18008, Spain

Maldonado R.F.:
 Instituto de Radioastronomía y Astrofísica, UNAM, Antigua Carretera A Pátzcuaro, 8701, Ex-Hda. San Jose de la Huerta, Mich, Morelia, 58089, Mexico

Chu Y.-H.:
 Institute of Astronomy and Astrophysics, Academia Sinica, No. 1, Section 4, Roosevelt Road, Taipei, 10617, Taiwan
ISSN: 00358711
Editorial
WILEY-BLACKWELL, COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA, Reino Unido
Tipo de documento: Article
Volumen: 527 Número: 3
Páginas: 6158-6172
WOS Id: 001116922000011
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