Published in

Cambridge University Press (CUP), Proceedings of the International Astronomical Union, S330(12), p. 317-320, 2017

DOI: 10.1017/s1743921317005427

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White dwarfs in the Gaia era

This paper was not found in any repository, but could be made available legally by the author.
This paper was not found in any repository, but could be made available legally by the author.

Full text: Unavailable

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Data provided by SHERPA/RoMEO

Abstract

AbstractThe vast majority of stars will become white dwarfs at the end of the stellar life cycle. These remnants are precise cosmic clocks owing to their well constrained cooling rates. Gaia Data Release 2 is expected to discover hundreds of thousands of white dwarfs, which can then be observed spectroscopically with WEAVE and 4MOST. By employing spectroscopically derived atmospheric parameters combined with Gaia parallaxes, white dwarfs can constrain the stellar formation history in the early developing phases of the Milky Way, the initial mass function in the 1.5 to 8 M range, and the stellar mass loss as well as the state of planetary systems during the post main-sequence evolution.

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