Weighing stars from birth to death : mass determination methods across the HRD
(2021) In Astronomy and Astrophysics Review 29(1).- Abstract
The mass of a star is the most fundamental parameter for its structure, evolution, and final fate. It is particularly important for any kind of stellar archaeology and characterization of exoplanets. There exist a variety of methods in astronomy to estimate or determine it. In this review we present a significant number of such methods, beginning with the most direct and model-independent approach using detached eclipsing binaries. We then move to more indirect and model-dependent methods, such as the quite commonly used isochrone or stellar track fitting. The arrival of quantitative asteroseismology has opened a completely new approach to determine stellar masses and to complement and improve the accuracy of other methods. We include... (More)
The mass of a star is the most fundamental parameter for its structure, evolution, and final fate. It is particularly important for any kind of stellar archaeology and characterization of exoplanets. There exist a variety of methods in astronomy to estimate or determine it. In this review we present a significant number of such methods, beginning with the most direct and model-independent approach using detached eclipsing binaries. We then move to more indirect and model-dependent methods, such as the quite commonly used isochrone or stellar track fitting. The arrival of quantitative asteroseismology has opened a completely new approach to determine stellar masses and to complement and improve the accuracy of other methods. We include methods for different evolutionary stages, from the pre-main sequence to evolved (super)giants and final remnants. For all methods uncertainties and restrictions will be discussed. We provide lists of altogether more than 200 benchmark stars with relative mass accuracies between [0.3 , 2] % for the covered mass range of M∈[0.1,16]M⊙, 75 % of which are stars burning hydrogen in their core and the other 25 % covering all other evolved stages. We close with a recommendation how to combine various methods to arrive at a “mass-ladder” for stars.
(Less)
- author
- organization
- publishing date
- 2021-12
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- Asteroseismology, Galaxy: stellar content, Methods: numerical, Stars: binaries: eclipsing, Stars: evolution, Stars: fundamental parameters, Stars: planetary systems
- in
- Astronomy and Astrophysics Review
- volume
- 29
- issue
- 1
- article number
- 4
- publisher
- Springer
- external identifiers
-
- scopus:85106966497
- ISSN
- 0935-4956
- DOI
- 10.1007/s00159-021-00132-9
- language
- English
- LU publication?
- yes
- additional info
- Publisher Copyright: © 2021, The Author(s), under exclusive licence to Springer-Verlag GmbH Germany, part of Springer Nature.
- id
- 02fae2de-d85b-4549-b912-c408f1a5444f
- date added to LUP
- 2022-03-10 11:17:53
- date last changed
- 2024-04-18 06:20:49
@article{02fae2de-d85b-4549-b912-c408f1a5444f, abstract = {{<p>The mass of a star is the most fundamental parameter for its structure, evolution, and final fate. It is particularly important for any kind of stellar archaeology and characterization of exoplanets. There exist a variety of methods in astronomy to estimate or determine it. In this review we present a significant number of such methods, beginning with the most direct and model-independent approach using detached eclipsing binaries. We then move to more indirect and model-dependent methods, such as the quite commonly used isochrone or stellar track fitting. The arrival of quantitative asteroseismology has opened a completely new approach to determine stellar masses and to complement and improve the accuracy of other methods. We include methods for different evolutionary stages, from the pre-main sequence to evolved (super)giants and final remnants. For all methods uncertainties and restrictions will be discussed. We provide lists of altogether more than 200 benchmark stars with relative mass accuracies between [0.3 , 2] % for the covered mass range of M∈[0.1,16]M⊙, 75 % of which are stars burning hydrogen in their core and the other 25 % covering all other evolved stages. We close with a recommendation how to combine various methods to arrive at a “mass-ladder” for stars.</p>}}, author = {{Serenelli, Aldo and Weiss, Achim and Aerts, Conny and Angelou, George C. and Baroch, David and Bastian, Nate and Beck, Paul G. and Bergemann, Maria and Bestenlehner, Joachim M. and Czekala, Ian and Elias-Rosa, Nancy and Escorza, Ana and Van Eylen, Vincent and Feuillet, Diane K. and Gandolfi, Davide and Gieles, Mark and Girardi, Léo and Lebreton, Yveline and Lodieu, Nicolas and Martig, Marie and Miller Bertolami, Marcelo M. and Mombarg, Joey S.G. and Morales, Juan Carlos and Moya, Andrés and Nsamba, Benard and Pavlovski, Krešimir and Pedersen, May G. and Ribas, Ignasi and Schneider, Fabian R.N. and Silva Aguirre, Victor and Stassun, Keivan G. and Tolstoy, Eline and Tremblay, Pier Emmanuel and Zwintz, Konstanze}}, issn = {{0935-4956}}, keywords = {{Asteroseismology; Galaxy: stellar content; Methods: numerical; Stars: binaries: eclipsing; Stars: evolution; Stars: fundamental parameters; Stars: planetary systems}}, language = {{eng}}, number = {{1}}, publisher = {{Springer}}, series = {{Astronomy and Astrophysics Review}}, title = {{Weighing stars from birth to death : mass determination methods across the HRD}}, url = {{http://dx.doi.org/10.1007/s00159-021-00132-9}}, doi = {{10.1007/s00159-021-00132-9}}, volume = {{29}}, year = {{2021}}, }