Implementing a Mass-Loss Model for Cool Stars in python
Research Mentor(s)
Kevin Covey
Description
The solar wind is composed of charged particles streaming away from the Sun at high velocity. Though much more difficult to detect directly, observations suggest other stars also drive these streams of particles. This continual outflow of matter means that stars with a stellar wind are losing mass, which can impact the star’s rotation rate as well as the atmospheres of its orbiting planets. Observations of our own Sun indicate magnetic Alfven waves and turbulence drive the Solar and stellar winds through such processes as hot corona gas pressure and cold-wave driven pressure waves. I translated the computational model by Cranmer & Saar (2011) designed to calculate the stellar mass-loss rates of cool stars (
Document Type
Event
Start Date
May 2022
End Date
May 2022
Location
Carver Gym (Bellingham, Wash.)
Department
CSE - Physics and Astronomy
Genre/Form
student projects; posters
Type
Image
Rights
Copying of this document in whole or in part is allowable only for scholarly purposes. It is understood, however, that any copying or publication of this document for commercial purposes, or for financial gain, shall not be allowed without the author’s written permission.
Language
English
Format
application/pdf
Implementing a Mass-Loss Model for Cool Stars in python
Carver Gym (Bellingham, Wash.)
The solar wind is composed of charged particles streaming away from the Sun at high velocity. Though much more difficult to detect directly, observations suggest other stars also drive these streams of particles. This continual outflow of matter means that stars with a stellar wind are losing mass, which can impact the star’s rotation rate as well as the atmospheres of its orbiting planets. Observations of our own Sun indicate magnetic Alfven waves and turbulence drive the Solar and stellar winds through such processes as hot corona gas pressure and cold-wave driven pressure waves. I translated the computational model by Cranmer & Saar (2011) designed to calculate the stellar mass-loss rates of cool stars (