Astronomy:HD 130948

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Short description: Star in the constellation Boötes
HD 130948
250px
The visual band light curve of HP Boötes, plotted from data published by Gaidos et al. (2000)[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Boötes[2]
Right ascension  14h 50m 15.8110s[3]
Declination +23° 54′ 42.634″[3]
Apparent magnitude (V) 5.99[4]
Characteristics
Evolutionary stage main sequence[3]
Spectral type F9 IV-V[5]
U−B color index +0.01[6]
B−V color index +0.576[4]
Variable type BY Dra[7]
Astrometry
Radial velocity (Rv)−1.5[8] km/s
Proper motion (μ) RA: +144.396[3] mas/yr
Dec.: +31.661[3] mas/yr
Parallax (π)54.9502 ± 0.0343[3] mas
Distance59.35 ± 0.04 ly
(18.20 ± 0.01 pc)
Absolute magnitude (MV)+4.56[2]
Details
Mass0.97[9] M☉
Radius1.1[3] R☉
Luminosity1.2[3] L☉
Surface gravity (log g)4.18[9] cgs
Temperature5,780[9] K
Metallicity [Fe/H]−0.20[9] dex
Rotation8.1[10]
Rotational velocity (v sin i)6.8[10] km/s
Age4.7[11] or 0.5[12] Gyr
Other designations
HP Boötis, GJ 564, BD+24°2786, HD 130948, FK5 3172, HIP 72567, HR 5534, SAO 83553[6]
Database references
SIMBADdata

HD 130948 or HP Boötis is a variable star with 2 brown dwarfs in the constellation Boötes. With an apparent magnitude of 6.0, it is faintly visible to the naked eye under very good observing conditions. It has a stellar classification of G1V, which means it is a main sequence star with a mass and surface temperature that are similar to the Sun.

The estimated age of HD 130948 is similar to the Sun at 4.7 billion years (Gyr) old, but it has a lower proportion of elements (63%) other than hydrogen or helium. However, a separate study in 2009 gave a much younger age of 0.5±0.3 Gyr and a higher metallicity that is very similar to the Sun.[12] Evolutionary models suggest that it is just reaching the end of its main sequence life.[3]

Eric J. Gaidos et al. observed the star in 1998 and 1999, and discovered that it is a variable star.[13] It was given its variable star designation, HP Boötis, in 2006.[7]

In 2002, a pair of co-orbiting brown dwarfs were discovered in orbit around this star. They were found using an adaptive optics instrument on the Gemini North 8m telescope in Hawaii.[14] The pair have a 10-year orbital period about the primary star, and their combined mass is 10.9% of the Sun's mass.[12]

The space velocity components of this star through the Milky Way galaxy are (U, V, W) = (−14.0, 14.7, −0.1).[9]

References

  1. ↑ Gaidos, E. J.; Henry, G. W.; Henry, S. M. (August 2000). "Spectroscopy and Photometry of Nearby Young Solar Analogs". The Astronomical Journal 120 (2): 1006–1013. doi:10.1086/301488. Bibcode: 2000AJ....120.1006G. 
  2. ↑ 2.0 2.1 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 3.8 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.
  4. ↑ 4.0 4.1 van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. 
  5. ↑ Gray, R. O.; Napier, M. G.; Winkler, L. I. (2001). "The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. I. Precise Spectral Types for 372 Stars". The Astronomical Journal 121 (4): 2148. doi:10.1086/319956. Bibcode: 2001AJ....121.2148G. 
  6. ↑ 6.0 6.1 "V* HP Boo -- Variable of BY Dra type". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD+130948. 
  7. ↑ 7.0 7.1 Kazarovets, E. V.; Samus, N. N.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (August 2006). "The 78th Name-List of Variable Stars". Information Bulletin on Variable Stars 5721: 1–45. Bibcode: 2006IBVS.5721....1K. https://ibvs.konkoly.hu/pub/ibvs/5701/5721.pdf. Retrieved 6 December 2024. 
  8. ↑ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". University of Toronto: International Astronomical Union. Bibcode: 1967IAUS...30...57E. 
  9. ↑ 9.0 9.1 9.2 9.3 9.4 Chen, Y. Q.; Nissen, P. E.; Zhao, G.; Zhang, H. W.; Benoni, T. (February 2000). "Chemical composition of 90 F and G disk dwarfs". Astronomy and Astrophysics Supplement 141 (3): 491–506. doi:10.1051/aas:2000124. Bibcode: 2000A&AS..141..491C. 
  10. ↑ 10.0 10.1 Bowler, Brendan P.; Tran, Quang H.; Zhang, Zhoujian; Morgan, Marvin; Ashok, Katelyn B.; Blunt, Sarah; Bryan, Marta L.; Evans, Analis E. et al. (2023). "Rotation Periods, Inclinations, and Obliquities of Cool Stars Hosting Directly Imaged Substellar Companions: Spin-Orbit Misalignments Are Common". The Astronomical Journal 165 (4): 164. doi:10.3847/1538-3881/acbd34. Bibcode: 2023AJ....165..164B. 
  11. ↑ Holmberg, J.; Nordstrom, B.; Andersen, J. (July 2009). "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics". Astronomy and Astrophysics 501 (3): 941–947. doi:10.1051/0004-6361/200811191. Bibcode: 2009A&A...501..941H. 
  12. ↑ 12.0 12.1 12.2 Dupuy, Trent J.; Liu, Michael C.; Ireland, Michael J. (February 2009). "Dynamical Mass of the Substellar Benchmark Binary HD 130948BC". The Astrophysical Journal 692 (1): 729–752. doi:10.1088/0004-637X/692/1/729. Bibcode: 2009ApJ...692..729D. 
  13. ↑ Gaidos, E. J.; Henry, G. W.; Henry, S. M. (August 2000). "Spectroscopy and Photometry of Nearby Young Solar Analogs". The Astronomical Journal 120 (2): 1006–1013. doi:10.1086/301488. Bibcode: 2000AJ....120.1006G. 
  14. ↑ Potter, Daniel; Martín, Eduardo L.; Cushing, Michael C.; Baudoz, Pierre; Brandner, Wolfgang; Guyon, Olivier; Neuhäuser, Ralph (March 2002). "Hokupa'a-Gemini Discovery of Two Ultracool Companions to the Young Star HD 130948". The Astrophysical Journal 567 (2): L133–L136. doi:10.1086/339999. Bibcode: 2002ApJ...567L.133P. 



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