Modeling Circumstellar Gas Emission around a White Dwarf Using cloudy

Abstract

The chemical composition of an extrasolar planet is fundamental to its formation, evolution, and habitability. In this study, we explore a new way to measure the chemical composition of the building blocks of extrasolar planets by measuring the gas composition of the disrupted planetesimals around white dwarf stars. As a first attempt, we used the photoionization code Cloudy to model the circumstellar gas emission around white dwarf Gaia J0611−6931 under some simplified assumptions. We found that most of the emission lines are saturated, and the line ratios approach the ratios of thermal emission; therefore, only lower limits to the number density can be derived. Silicon is the best-constrained element in the circumstellar gas, and we derived a lower limit of 10 ^10.3 cm ^−3 . In addition, we placed a lower limit on the total amount of gas to be 1.8 × 10 ^19 g. Further study is needed to better constrain the parameters of the gas disk and connect it to other white dwarfs with circumstellar gas absorption.

Keywords

• Circumstellar gas
• Chemical abundances
• Debris disks
• Planetesimals
• Extrasolar rocky planets
• White dwarf stars