Classical nova explosions

TL;DR

This review discusses the current understanding of classical nova explosions, focusing on nucleosynthesis, observational signatures, and modeling challenges to better comprehend these stellar phenomena.

Contribution

It synthesizes recent advances in nova modeling, emphasizing nucleosynthetic products, observational constraints, and critical modeling issues, highlighting areas for future research.

Findings

Nucleosynthetic yields depend on white dwarf properties.

Gamma-ray observations can constrain nova models.

Understanding mixing mechanisms is crucial for accurate modeling.

Abstract

A review of the present status of nova modeling is made, with a special emphasis on some specific aspects. What are the main nucleosynthetic products of the explosion and how do they depend on the white dwarf properties (e.g. mass, chemical composition: CO or ONe)? What's the imprint of nova nucleosynthesis on meteoritic presolar grains? How can gamma rays, if observed with present or future instruments onboard satellites, constrain nova models through their nucleosynthesis? What have we learned about the turnoff of classical novae from observation with past and present X-ray observatories? And last but not least, what are the most critical issues concerning nova modeling (e.g. ejected masses, mixing mechanism between core and envelope)?