Astronomy:BD-11 4672

From HandWiki
Short description: Orange dwarf in the constellation Scutum
BD-11 4672
Observation data
Epoch J2000.0   Equinox (celestial coordinates)
Constellation Scutum[1]
Right ascension  18h 33m 28.832s[2]
Declination −11° 38′ 09.72″[2]
Apparent magnitude (V) 9.99±0.05[3]
Characteristics
Evolutionary stage main sequence[3]
Spectral type K7 V[4][3]
Apparent magnitude (B) 11.21±0.10[3]
Apparent magnitude (J) 7.651±0.023[1]
B−V color index 1.263±0.009[1]
Astrometry
Radial velocity (Rv)−87.515±0.0011[5] km/s
Proper motion (μ) RA: −288.440[2] mas/yr
Dec.: −235.615[2] mas/yr
Parallax (π)36.7534 ± 0.0157[2] mas
Distance88.74 ± 0.04 ly
(27.21 ± 0.01 pc)
Details
Mass0.651+0.031−0.029[3] M☉
Radius0.639+0.020−0.022[3] R☉
Luminosity0.157+0.019−0.017[3] L☉
Surface gravity (log g)4.642+0.027−0.025[3] cgs
Temperature4,550±110[3] K
Metallicity [Fe/H]−0.48±0.07[6] dex
Rotation~25 d[3]
Rotational velocity (v sin i)1.0±0.5[3] km/s
Age7.4+4.5−4.9[3] Gyr
Other designations
BD−11 4672, Gaia DR2 4154598526336121600, GJ 717, HIP 90979, PPM 234703, Wolf 1462, TYC 5699-2129-1, GSC 05699-02129, 2MASS J18332885-1138097[7]
Database references
SIMBADdata

BD−11 4672 is a single star with a pair of orbiting exoplanets in the southern constellation of Scutum, the shield. The designation BD−11 4672 comes from the Bonner Durchmusterung star catalogue, which was published during the nineteenth century in Germany. With an apparent visual magnitude of 9.99,[3] the star is much too faint to be viewed with the naked eye. It is located at a distance of 89 light years from the Sun, as determined from parallax,[2] but is drifting closer with a radial velocity of −87.5 km/s.[5] This was recognised as a high proper motion star by German astronomer Max Wolf in 1924[8] and is traversing the celestial sphere at an angular rate of 0.401 arcsec yr−1.[9]

The spectrum of BD−11 4672 matches a K-type main-sequence star, an orange dwarf, with a stellar classification of K7 V.[4] Its age is not well constrained, but is probably older than the Sun. It is a metal-poor star, showing an iron abundance that is 35% of solar.[6] No significant flare activity was detected.[10] The star shows evidence of a Sun-like magnetic activity cycle with a period of 7–10 years.[3] It has 65% of the mass and 64% of the radius of the Sun. The star is radiating 16% of the luminosity of the Sun from its photosphere at an effective temperature of 4,550 K.[3]

Planetary system

In 2010, a team of astronomers led by astronomer C. Moutou of the High Accuracy Radial Velocity Planet Searcher performed a radial-velocity analysis, which led to the suspicion of a gas giant exoplanet in orbit around BD−11 4672.[4] The existence of this exoplanet was confirmed in 2014.[11] In 2020, a second exoplanet was detected on an interior and much more eccentric orbit near the inner edge of the Star's habitable zone.[3]

The BD-11 4672 planetary system[12][3]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b >0.65±0.05 MJ 2.36±0.04 1634±14 0.05±0.05 — —
c >0.04836+0.009−0.0066 MJ 0.3±0.01 74.2±0.08 0.4±0.15 — —

See also

References

  1. ↑ 1.0 1.1 1.2 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  3. ↑ 3.00 3.01 3.02 3.03 3.04 3.05 3.06 3.07 3.08 3.09 3.10 3.11 3.12 3.13 3.14 3.15 3.16 Barbato, D. et al. (2020), "The GAPS Programme at TNG XXIV. An eccentric Neptune-mass planet near the inner edge of the BD-11 4672 habitable zone", Astronomy & Astrophysics A68: 641, doi:10.1051/0004-6361/202037954, Bibcode: 2020A&A...641A..68B. 
  4. ↑ 4.0 4.1 4.2 Moutou, Claire et al. (March 2011), "The HARPS search for southern extra-solar planets: XXVI: Seven new planetary systems", Astronomy & Astrophysics 527, doi:10.1051/0004-6361/201015371, A63, Bibcode: 2011A&A...527A..63M. 
  5. ↑ 5.0 5.1 Soubiran, C. et al. (2018), "Gaia Data Release 2. The catalogue of radial velocity standard stars", Astronomy and Astrophysics 616: A7, doi:10.1051/0004-6361/201832795, Bibcode: 2018A&A...616A...7S. 
  6. ↑ 6.0 6.1 Andreasen, D. T. et al. (2017), "SWEET-Cat update and FASMA A new minimization procedure for stellar parameters using high-quality spectra", Astronomy & Astrophysics A69: 600, doi:10.1051/0004-6361/201629967, Bibcode: 2017A&A...600A..69A. 
  7. ↑ "BD-11 4672". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=BD-11+4672. 
  8. ↑ Wolf, M.; Reinmuth, K. (1925), "Einige bewegte Sterne in Scutum", Astronomische Nachrichten 223 (14): 231, doi:10.1002/asna.19242231404, Bibcode: 1925AN....223..231W. 
  9. ↑ Luyten, W. J. (June 1995), "NLTT Catalogue (Luyten, 1979)", VizieR Online Data Catalog, Bibcode: 1995yCat.1098....0L. 
  10. ↑ Lammer, H. et al. (2020), "A census of Coronal Mass Ejections on solar-like stars", Monthly Notices of the Royal Astronomical Society 493 (3): 4570–4589, doi:10.1093/mnras/staa504, Bibcode: 2020MNRAS.493.4570L. 
  11. ↑ Moutou, C. et al. (2014), "The HARPS search for southern extra-solar planets", Astronomy & Astrophysics 576: A48, doi:10.1051/0004-6361/201424965, Bibcode: 2015A&A...576A..48M. 
  12. ↑ Planet BD-11 4672 b, https://exoplanet.eu/catalog/bd_11_4672_b--796/, retrieved 2024-01-05. 

Coordinates: Sky map 18h 33m 28.8323s, −11° 38′ 09.7218″



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:BD-11_4672&oldid=3354986"