USNO: Astronomers Resolve Mystery of White Dwarf's Mass

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USNO: Astronomers Resolve Mystery of White Dwarf's Mass

Postby bystander » Tue Sep 12, 2017 2:33 am

Astronomers Resolve Mystery of White Dwarf's Mass
US Naval Observatory | phys.org | 2017 Sep 11

New observations of the white dwarf/red dwarf binary star 40 Eridani BC by astronomers at the U.S. Naval Observatory (USNO) have revealed new, definitive values for the orbital period and masses of the components of this interesting stellar pair. A paper describing the observations and the results by Dr. Brian Mason, Dr. Bill Hartkopf, and intern Korie Miles has been accepted for publication in the Astronomical Journal.

40 Eridani BC (also known as Omicron-2 Eridani) is a well-known double star that has been observed by many astronomers since its properties were first accurately measured by William Rutter Dawes in 1867. It is located about 16 light-years from Earth and is easily observed in amateur telescopes. Measuring the period of the component stars as they orbit their center of mass and knowing their distance allows astronomers to compute their combined masses. As more observations were recorded over the decades, the characteristics of the stars' orbits were computed, allowing a first determination of the stars' combined masses. It quickly became apparent that 40 Eridani BC was an unusual system.

By combining the computed orbits with spectrographic data and the stars' nearby location, it was found that the brighter component was a "white dwarf," the highly compressed remnant of a star that has collapsed after exhausting its nuclear fuel. The fainter component is a "red dwarf," a low-luminosity, low-mass star that will feebly shine for hundreds of billions of years. While red dwarf stars may be the most prevalent types of "normal" stars in the galaxy, white dwarf stars are comparatively rare. 40 Eridani B is the second-brightest white dwarf known and is the only one that can easily be seen in backyard telescopes. It was also the first white dwarf star to have its mass determined by measuring its gravitational redshift, a characteristic of very dense objects. ...

Binary Star Orbits. V. The Nearby White Dwarf - Red Dwarf pair 40 Eri BC - Brian D. Mason, William I. Hartkopf, Korie N. Miles
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Re: USNO: Astronomers Resolve Mystery of White Dwarf's Mass

Postby MargaritaMc » Tue Sep 12, 2017 12:12 pm

https://arxiv.org/abs/1709.00478
Astrophysical Implications of a New Dynamical Mass for the Nearby White Dwarf 40 Eridani B

Howard E. Bond (1,2), P. Bergeron (3), A. Bedard (3) ((1) Penn State Univ., (2) Space Telescope Science Institute, (3) Departement de Physique, Univ. de Montreal)
(Submitted on 1 Sep 2017)
The bright, nearby DA-type white dwarf (WD) 40 Eridani B is orbited by the M dwarf 40 Eri C, allowing determination of the WD's mass. Until recently, however, the mass depended on orbital elements determined four decades ago, and that mass was so low that it created several astrophysical puzzles. Using new astrometric measurements, the binary-star group at the U.S. Naval Observatory has revised the dynamical mass upward,


https://astrobites.org/2017/09/12/40-er ... ging-star/
40 Eridani B: a Challenging Star, by Ingrid Pelisoli | Sep 12, 2017
"In those rare moments of total quiet with a dark sky, I again feel the awe that struck me as a child. The feeling is utterly overwhelming as my mind races out across the stars. I feel peaceful and serene."
— Dr Debra M. Elmegreen, Fellow of the AAAS


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