BD−08°2823

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BD−08°2823
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Sextans
Right ascension 10h 00m 47.7206s [1]
Declination –09° 31′ 00.0428″ [1]
Apparent magnitude  (V)9.86 [2]
Characteristics
Spectral type K4:V [3]
Apparent magnitude  (B)10.931 [2]
Apparent magnitude  (J)7.960±0.020 [2]
Apparent magnitude  (H)7.498±0.047 [2]
Apparent magnitude  (K)7.323±0.021 [2]
B−V color index 1.071±0.010 [2]
Astrometry
Radial velocity (Rv)53.47±0.19 [1]  km/s
Proper motion (μ)RA: −375.517±0.066  mas/yr [1]
Dec.: 25.460±0.060  mas/yr [1]
Parallax (π)24.1641 ± 0.0397  mas [1]
Distance 135.0 ± 0.2  ly
(41.38 ± 0.07  pc)
Absolute magnitude  (MV)6.73 [2]
Details
Mass 0.741±0.020 [4]   M☉
Radius 0.71±0.04 [5]   R☉
Luminosity 0.237±0.001 [1]   L☉
Surface gravity (log g)4.33±0.26 [6]   cgs
Temperature 4,746±63 [7]   K
Metallicity [Fe/H]−0.04±0.06 [4]   dex
Rotation 26.6±1.5  days [7]
Rotational velocity (v sin i)1.4 [7]  km/s
Age 5.0±4.7 [4]   Gyr
Other designations
BD−08°2823, Gaia DR2  3770419611540574080, HIP  49067, SAO  137286, PPM  192987, LTT  3669, NLTT  23181, Ross  444 [8]
Database references
SIMBAD data
Exoplanet Archive data
Extrasolar Planets
Encyclopaedia 		data

BD−08°2823 is a star with a pair of exoplanetary companions in the faint equatorial constellation of Sextans. The star has an apparent visual magnitude of 9.86, [2] which is too faint to be visible with the naked eye. This system is located at a distance of 135  light-years from the Sun based on parallax measurements, and is trending further away with a radial velocity of +53 km/s. [1] It is a high proper motion star that is traversing the celestial sphere at the angular rate of 0.369″ yr−1. [9]

Contents

This is an ordinary K-type main-sequence star with a stellar classification of K4:V, [3] where the ':' notation indicates some uncertainty. Emission cores in the H and K lines suggest this is an active star, with the level of activity varying significantly over time. [7] It is roughly five billion years old [4] and is spinning with a projected rotational velocity of 1.4 km/s. [7] Measurements of the activity variation suggest a rotation period of around 27  days. [7] This star is smaller, cooler, and less massive than the Sun. Its metal content is slightly lower than in the Sun. [4] The star is radiating 24% of the luminosity of the Sun from its photosphere at an effective temperature of 4,746 K. [7]

Planetary system

In 2009, two planets were found in orbit around the star. They were discovered using the radial velocity method with the HARPS spectrograph in Chile, despite the data noise introduced through surface activity. The inner planet has a minimum mass equal to 14.4±2.1 times the mass of the Earth, while the outer planet is at least one third the mass of Jupiter. [7]

The BD−08°2823 planetary system [7]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥0.045 ± 0.007  MJ 0.056 ± 0.0025.60 ± 0.020.15 ± 0.15——
c ≥0.33 ± 0.03  MJ 0.68 ± 0.02237.6 ± 1.50.19 ± 0.09——

See also

Related Research Articles

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HD 8535 is a star located 181 light years away from the Sun in the southern constellation of Phoenix. It has a yellow hue and can be viewed using binoculars or a small telescope, having a low apparent visual magnitude of 7.70. The star is drifting further away from the Sun with a radial velocity of +2.4 km/s.

HD 44219 is a solar-type star with an exoplanetary companion in the equatorial constellation of Monoceros. It has an apparent visual magnitude of 7.69, making it an 8th magnitude star that is too faint to be readily visible to the naked eye. The system is located at a distance of 173 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −12 km/s.

HD 9578 is a candidate wide binary star system located at a distance of approximately 183 light-years from the Sun in the southern constellation of Sculptor. The main star must be viewed with binoculars or a telescope, as its low apparent visual magnitude of 8.35 is too faint to be viewed with the naked eye. The system is drifting closer to the Sun with a radial velocity of −4 km/s.

HD 103197 is a star with a planetary companion in the southern constellation of Centaurus. It has an apparent visual magnitude of 9.40, which is too faint to be viewed with the naked eye. Based on parallax measurements, HD 103197 is located at a distance of 187 light years from the Sun. It is drifting closer with a radial velocity of −4.6 km/s.

HD 103774 is a star with a close orbiting planetary companion in the southern constellation of Corvus. With an apparent visual magnitude of 7.13, it is too faint to be readily visible to the naked eye. Parallax measurements provide a distance estimate of 184 light years from the Sun. It is drifting closer with a radial velocity of −3 km/s. The star has an absolute magnitude of 3.41.

HD 44120 is a wide binary star system in the southern constellation of Pictor. Although visible to the naked eye, it is a challenge to view having an apparent visual magnitude of 6.44. The system is located at a distance of 118 light years from the Sun based on parallax, but it is drifting closer with a radial velocity of −2 km/s. It has an absolute magnitude of 3.57.

References

  1. 1 2 3 4 5 6 7 8 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  2. 1 2 3 4 5 6 7 8 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID   119257644.
  3. 1 2 Stephenson, C. B. (July 1986). "Dwarf K and M stars of high proper motion found in a hemispheric survey". Astronomical Journal. 92: 139–165. Bibcode:1986AJ.....92..139S. doi: 10.1086/114146 .
  4. 1 2 3 4 5 Delgado Mena, E.; et al. (April 2019). "Abundance to age ratios in the HARPS-GTO sample with Gaia DR2. Chemical clocks for a range of [Fe/H]". Astronomy & Astrophysics. 624: 24. arXiv: 1902.02127 . Bibcode:2019A&A...624A..78D. doi:10.1051/0004-6361/201834783. S2CID   90259810. A78.
  5. ↑ Stassun, Keivan G.; et al. (2016). "Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes". The Astronomical Journal. 153 (3): 136. arXiv: 1609.04389 . Bibcode:2017AJ....153..136S. doi: 10.3847/1538-3881/aa5df3 . S2CID   119219062.
  6. ↑ Delgado Mena, E.; et al. (October 2017). "Chemical abundances of 1111 FGK stars from the HARPS GTO planet search program. II. Cu, Zn, Sr, Y, Zr, Ba, Ce, Nd, and Eu". Astronomy & Astrophysics. 606: 20. arXiv: 1705.04349 . Bibcode:2017A&A...606A..94D. doi:10.1051/0004-6361/201730535. S2CID   118908425. A94.
  7. 1 2 3 4 5 6 7 8 9 Hébrard, G.; et al. (2010). "The HARPS search for southern extra-solar planets XX. Planets around the active star BD -08°2823". Astronomy and Astrophysics. 512. A46. arXiv: 0912.3202 . Bibcode:2010A&A...512A..46H. doi:10.1051/0004-6361/200913525. S2CID   73713738.
  8. ↑ "BD-08 2823". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2021-11-14.
  9. ↑ Luyten, W. J. (June 1995). "NLTT Catalogue". VizieR Online Data Catalog. Bibcode:1995yCat.1098....0L.
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