Xi Bootes

ξ Bootes
ξ Bootes
	Star
Observational data; ( Age J2000.0 )
Right ascension
Declination
Distance	22.1 ± 0.1 St. years (6.78 ± 0.03 pc )
Visible magnitude ( V )	A: 4.70 ; B: 6.97
Constellation	Bootes
Astrometry
Radial velocity ( R v )	3.0 km / s
Own movement (μ)	RA: 152.81 mas per year; Dec: -71.28 mas per year
Parallax (π)	149.26 ± 0.76 mas
Absolute magnitude (V)	A: 5.54 ; B: 7.81
Specifications
Spectral class	A: G8Ve ; B: K4Ve
Variability	A: BY Dra ; B: flashing
physical characteristics
Weight	0.9 / 0.7 M ☉
Radius	0.89 / 0.71 R ☉
Temperature	5128K / 3410 K
Luminosity	0.49 / 0.061 L ☉
Metallicity	A: 55-155% ; B:?
Rotation	A: 3 km / s; B:?
Other designations
	37 Bootes, Gliese 566, Xi Boötis, 37 Boötis, Gl 566, HR 5544, BD +19 2870, HD 131156, GCTP 3360.00, SAO 101250, Struve 1888, ADS 9413, GC 19991, CCDM 14513 + 1906, HIP 72659 ;
Database Information
SIMBAD	data
ARICNS	data

Xi Boopas ( lat.Xi Boötis ) is a binary star located in the constellation Bootes at a distance of about 22 light-years from us.

Content

Features

The Bootes ξ system is visible to the naked eye as a dim orange star. Her research has been ongoing for a long time. In 1780, the English astronomer William Herschel discovered the presence of the second component of the star. According to new, refined measurements, the components are separated by a distance of 33.6 a. e. (4.94 "), making a complete revolution around the common center of mass in 151.6 years. Stars move in an elongated elliptical orbit (e = 0.51) with an apoaster of 16.5 a.u. and a periastron of 50.7 a that is, ^[1] In 1943, the Danish astronomer Kaj Arand Gunnar Strand announced the discovery of systematic oscillations in the radial velocity ξ of Bootes, which he observed from 1939 to 1942. These astrometric oscillations made it possible to make the assumption that in the system is subzvozdny object weighing about 1/10 of the solar mass. In 1988 godu group astronomers confirmed the existence of periodic count -oscillations in the radial velocity, which indicates the possible existence of a companion weighing in 1-9 mass of Jupiter orbiting the star ξ Bootes B. ^[2] However, the exact evidence of the existence of the object has yet been found.

ξ Bootes A

The main component is a yellow dwarf , in its characteristics resembling the Sun. The mass and diameter of the star are 90–94% and 89% of the solar, respectively ^[3] and the luminosity is only 49% of the solar luminosity. Since the star has violent chromospheric activity, this means that she is quite young by astronomical standards: her age is estimated at 60 million years. ^{[4] The} activity of the stellar interior is the cause of variability : the brightness ξ of Bootes A varies between 4.52 and 4.67 of the apparent stellar magnitude with a frequency of every 10.13 days, which classifies it as variables of the Dragon BY type.

ξ Bootes B

The second component is a fainter and relatively cold star (3410 degrees Kelvin on the surface) and belongs to the class of orange dwarfs of the main sequence. Its mass is approximately equal to 67–76% of the sun , and its diameter is equivalent to 71% of the diameter of the sun. ^[3]

Nearest star environment

The following stellar systems are located within 10 light years of Bootes ξ:

Star	Spectral class	Distance, st. years old
Laland 25372	M1.5 Ve	6.9
BD + 11 2576	M1 V	9.2
LP 378-541	M2 V	9.3

Notes

↑ Söderhjelm, Staffan. Visual binary orbits and masses POST HIPPARCOS . Astronomy and Astrophysics, v. 341, p. 121-140 (1999) (01/1999). Date of treatment September 21, 2009. Archived April 1, 2012.
↑ Campbell, B., Walker, GAH, & Yang, S. A search for substellar companions to solar-type stars . Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 331, Aug. 15, 1988, p. 902-921. (Aug. 15, 1988). Date of treatment September 21, 2009. Archived on April 7, 2012.
↑ ¹ ² Johnson, HM & Wright, CD redicted infrared brightness of stars within 25 parsecs of the sun . Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 53, Nov. 1983, p. 643-711. (Nov. 1983). Date of treatment September 21, 2009. Archived February 16, 2012.
↑ Barry, DC The chromospheric age dependence of the birthrate, composition, motions, and rotation of late F and G dwarfs within 25 parsecs of the sun . Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 334, Nov. 1, 1988, p. 436-448. (Nov. 1, 1988). Date of treatment September 21, 2009. Archived on April 7, 2012.

Links

Solstation

[1] Söderhjelm, Staffan. Visual binary orbits and masses POST HIPPARCOS . Astronomy and Astrophysics, v. 341, p. 121-140 (1999) (01/1999). Date of treatment September 21, 2009. Archived April 1, 2012.

[2] Campbell, B., Walker, GAH, & Yang, S. A search for substellar companions to solar-type stars . Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 331, Aug. 15, 1988, p. 902-921. (Aug. 15, 1988). Date of treatment September 21, 2009. Archived on April 7, 2012.

[Johnson_and_Wright,_1983-3] ¹ ² Johnson, HM & Wright, CD redicted infrared brightness of stars within 25 parsecs of the sun . Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 53, Nov. 1983, p. 643-711. (Nov. 1983). Date of treatment September 21, 2009. Archived February 16, 2012.

[4] Barry, DC The chromospheric age dependence of the birthrate, composition, motions, and rotation of late F and G dwarfs within 25 parsecs of the sun . Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 334, Nov. 1, 1988, p. 436-448. (Nov. 1, 1988). Date of treatment September 21, 2009. Archived on April 7, 2012.