Bayesian Inference for the White Dwarf Initial-Final Mass Relation

Nathan Stein; Ted von Hippel; David van Dyk; Steven DeGennaro; Elizabeth Jeffery; Bill Jefferys

Bayesian Inference for the White Dwarf Initial-Final Mass Relation

Nathan Stein
, Ted von Hippel
, David van Dyk
, Steven DeGennaro
, Elizabeth Jeffery
, Bill Jefferys

Harvard University
Siena College
University of California, Irvine
The University of Texas, Austin
Space Telescope Science Institute
University of Texas, University of Vermont

Research output: Contribution to conference › Presentation

Abstract

Stars lose mass as they age, and understanding mass loss is important for understanding stellar evolution. The initial-final mass relation (IFMR) is the relationship between a white dwarf’s initial mass on the main sequence and its final mass. We have developed a new method for fitting the IFMR based on a Bayesian analysis of photometric observations, combining deterministic models of stellar evolution in an internally coherent way. No mass data are used. Our method yields precise inferences (with uncertainties) for a parameterized linear IFMR. Our method can also return posterior distributions of white dwarf initial and final masses.

Original language	American English
State	Published - Jul 2023
Externally published	Yes

Keywords

main-sequence stars
stellar evolution

Disciplines

Stars, Interstellar Medium and the Galaxy

Access to Document

Bayesian Inference for the White Dwarf Initial-Final Mass RelatioFinal published version, 835 KBLicense: CC BY

Cite this

@conference{9c7138b0ceb74e6098ef2c1c8ac07d9a,

title = "Bayesian Inference for the White Dwarf Initial-Final Mass Relation",

abstract = " Stars lose mass as they age, and understanding mass loss is important for understanding stellar evolution. The initial-final mass relation (IFMR) is the relationship between a white dwarf{\textquoteright}s initial mass on the main sequence and its final mass. We have developed a new method for fitting the IFMR based on a Bayesian analysis of photometric observations, combining deterministic models of stellar evolution in an internally coherent way. No mass data are used. Our method yields precise inferences (with uncertainties) for a parameterized linear IFMR. Our method can also return posterior distributions of white dwarf initial and final masses.",

keywords = "main-sequence stars, stellar evolution",

author = "Nathan Stein and Hippel, \{Ted von\} and Dyk, \{David van\} and Steven DeGennaro and Elizabeth Jeffery and Bill Jefferys",

year = "2023",

month = jul,

language = "American English",

}

TY - CONF

T1 - Bayesian Inference for the White Dwarf Initial-Final Mass Relation

AU - Stein, Nathan

AU - Hippel, Ted von

AU - Dyk, David van

AU - DeGennaro, Steven

AU - Jeffery, Elizabeth

AU - Jefferys, Bill

PY - 2023/7

Y1 - 2023/7

N2 - Stars lose mass as they age, and understanding mass loss is important for understanding stellar evolution. The initial-final mass relation (IFMR) is the relationship between a white dwarf’s initial mass on the main sequence and its final mass. We have developed a new method for fitting the IFMR based on a Bayesian analysis of photometric observations, combining deterministic models of stellar evolution in an internally coherent way. No mass data are used. Our method yields precise inferences (with uncertainties) for a parameterized linear IFMR. Our method can also return posterior distributions of white dwarf initial and final masses.

AB - Stars lose mass as they age, and understanding mass loss is important for understanding stellar evolution. The initial-final mass relation (IFMR) is the relationship between a white dwarf’s initial mass on the main sequence and its final mass. We have developed a new method for fitting the IFMR based on a Bayesian analysis of photometric observations, combining deterministic models of stellar evolution in an internally coherent way. No mass data are used. Our method yields precise inferences (with uncertainties) for a parameterized linear IFMR. Our method can also return posterior distributions of white dwarf initial and final masses.

KW - main-sequence stars

KW - stellar evolution

UR - https://commons.erau.edu/publication/2047

M3 - Presentation

ER -

Bayesian Inference for the White Dwarf Initial-Final Mass Relation

Abstract

Keywords

Disciplines

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