Abstract
Classical nova explosions and type I X-ray bursts are the most frequent types of thermonuclear stellar explosions in the Galaxy. Both phenomena arise from thermonuclear ignition in the envelopes of accreting compact objects in close binary star systems. Detailed observations of these events have stimulated numerous studies in theoretical astrophysics and experimental nuclear physics. We discuss observational features of these phenomena and theoretical efforts to better understand the energy production and nucleosynthesis in these explosions. We also examine and summarize studies directed at identifying nuclear physics quantities with uncertainties that significantly affect model predictions.
Highlights
The first systematic registry of novae was initiated around 200 BCE by officials of the Chinese imperial court
The first X-ray burst was identified in 19752 from a previously-known X-ray source, 4U 1820-30. [Note that most X-ray sources are named using letters from the satellites that discovered them (e.g., 4U stands for the 4th catalogue of the satellite Uhuru, the first satellite dedicated to X-ray astronomy), and numbers corresponding to their coordinates in Right Ascension (e.g., 1820 stands for 18h 20min) and Declination (–30 deg) in the sky
We will focus on standard models of classical nova explosions (CN) and models of X-ray bursts (XRBs) that occur in envelopes containing substantial H and He
Summary
The first systematic registry of novae was initiated around 200 BCE by officials of the Chinese imperial court (see Duerbeck for a list of observed novae up to 1604). Calculations indicate that radiative winds generated during some bursts may eject material; studies are ongoing to examine the viability of detecting absorption features arising from this material Both classical nova explosions (CN) and type I X-ray bursts (XRBs) arise from thermonuclear runaways within the accreted envelopes of compact objects in close binary systems, with orbital periods often less than 15 hours. The framework of this article reflects the approach requested by the editors, namely, to address less what is known, and more what is as yet unknown by discussing questions that still need answering and which methods are the most powerful for doing so In this vein, we present below four headings regarding needs to better constrain predictions from models of classical novae and type I X-ray bursts. We certainly do not claim to have summarized all the varied outstanding problems and challenges that remain for these phenomena. (For example, we do not discuss the unexplained oscillations observed in the light curves of XRBs9,11,12 or in the soft X-ray light curves from novae, both of which may be indicative of a confined radiating region.) the issues discussed below represent major tasks or obstacles that need to be addressed to improve our understanding of these thermonuclear explosions
Sign-in/Register to view highlights & summary Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
