X-ray observations of the nova shell IPHASX J210204.7+471015
Abstract
We present the analysis of XMM-Newton European Photon Imaging Camera (EPIC) observations of the nova shell IPHASX J210204.7+471015. We detect X-ray emission from the progenitor binary star with properties that resemble those of underluminous intermediate polars such as DQ Herculis (DQ Her): an X-ray-emitting plasma with temperature of TX = (6.4 ± 3.1) × 106 K, a non-thermal X-ray component, and an estimated X-ray luminosity of LX = 1030 erg s-1. Time series analyses unveil the presence of two periods, the dominant with a period of 2.9 ± 0.2 h, which might be attributed to the spin of the white dwarf, and a secondary of 4.5 ± 0.6 h that is in line with the orbital period of the binary system derived from optical observations. We do not detect extended X-ray emission as in other nova shells probably due to its relatively old age (130-170 yr) or to its asymmetric disrupted morphology that is suggestive of explosion scenarios different to the symmetric ones assumed in available numerical simulations of nova explosions.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- April 2021
- DOI:
- 10.1093/mnras/stab273
- arXiv:
- arXiv:2101.11480
- Bibcode:
- 2021MNRAS.502.4658T
- Keywords:
-
- binaries: general;
- stars: evolution;
- novae;
- cataclysmic variables;
- X-rays: individual: IPHASX J 210204.7+471015;
- X-rays: stars;
- transients: novae;
- Astrophysics - Solar and Stellar Astrophysics;
- Astrophysics - High Energy Astrophysical Phenomena
- E-Print:
- 6 pages and 5 Figures