X-ray observations of classical novae. Theoretical implications

Abstract

Detection of X-rays from classical novae, both in outburst and post-outburst, provides unique and crucial information about the explosion mechanism. Soft X-rays reveal the hot white dwarf photosphere, whenever hydrogen (H) nuclear burning is still on and expanding envelope is transparent enough, whereas harder X-rays give information about the ejecta and/or the accretion flow in the reborn cataclysmic variable. The duration of the supersoft X-ray emission phase is related to the turn-off of the classical nova, i.e., of the H-burning on top of the white dwarf core. A review of X-ray observations is presented, with a special emphasis on the implications for the duration of post-outburst steady H-burning and its theoretical explanation. The particular case of recurrent novae (both the "standard" objects and the recently discovered ones) is also reviewed, in terms of theoretical feasibility of short recurrence periods, as well as regarding implications for scenarios of type Ia supernovae.

6 pages, review paper accepted for publication in Astronomische Nachrichten

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Cited by in corpus (9)

• Swift X-Ray Observations of Classical Novae. II. The Super Soft Source sample
• Observations of Galactic and Extragalactic Novae
• Revisiting the ultraluminous supersoft source in M101: an optically thick outflow model
• External Mass Accumulation onto Core Potentials: Implications for Star Clusters, Galaxies and Galaxy Clusters
• X-ray Spectroscopy of the gamma-ray Brightest Nova V906 Car (ASASSN-18fv)
• The multi-wavelength view of shocks in the fastest nova V1674 Her
• X-ray observations of historical classical nova counterparts with eROSITA telescope aboard SRG orbital observatory during the all-sky survey
• The supersoft X-ray source in V5116 Sgr I. The high resolution spectra
• X-ray observations of the nova shell IPHASX J210204.7+471015