Astronomy:HD 177406

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Short description: Star in the constellation of Telescopium
HD 177406
Location of HD 177406 (circled)
Observation data
Epoch J2000.0   Equinox (celestial coordinates)
Constellation Telescopium
Right ascension  19h 06m 55.60698s[1]
Declination −48° 17′ 56.9195″[1]
Apparent magnitude (V) 5.95±0.01[2]
Characteristics
Evolutionary stage main sequence star[1]
Spectral type A0 V[3]
U−B color index −0.02[4]
B−V color index −0.01[4]
Astrometry
Radial velocity (Rv)−6.2±1.6[5] km/s
Proper motion (μ) RA: +13.500[1] mas/yr
Dec.: −12.738[1] mas/yr
Parallax (π)8.8414 ± 0.0541[1] mas
Distance369 ± 2 ly
(113.1 ± 0.7 pc)
Absolute magnitude (MV)+0.60[6]
Details
Mass2.64+0.43−0.28[7] M☉
Radius2.55±0.13[8] R☉
Luminosity62.4+1.5−1.4[1] L☉
Surface gravity (log g)4.00[9] cgs
Temperature10,275+229−194[7] K
Metallicity [Fe/H]0.00[10] dex
Rotation27.2 d[11]
Rotational velocity (v sin i)50 - 100[12] km/s
Age286±9[13][10] Myr
Other designations
CD−48°12901, CPD−48°10045, FK5 3523, GC 26272, HD 177406, HIP 93862, HR 7223, SAO 229493[14]
Database references
SIMBADdata

HD 177406, also known as HR 7223 or rarely 47 G. Telescopii, is a solitary star[15] located in the southern constellation Telescopium. It is faintly visible to the naked eye as a white-hued point of light with an apparent magnitude of 5.95.[2] Gaia DR3 parallax measurements imply a distance of 369 light years[1] and it is currently approaching the Solar System with a heliocentric radial velocity of −6.2 km/s.[5] At its current distance, HD 177406's brightness is diminished by 0.23 magnitudes due to interstellar dust[16] and it has an absolute magnitude of +0.60.[6]

HD 177406 has a stellar classification of A0 V,[3] indicating that it is an ordinary A-type main-sequence star that is generating energy via hydrogen fusion at its core. It has 2.64 times the mass of the Sun[7] and a radius 2.55 times that of the Sun.[8] It radiates 62.4 times the luminosity of the Sun[1] from its photosphere at an effective temperature of 10,275 K.[7] It has a solar metallicity at [Fe/H] = +0.00 and it is estimated to be 286 million years old,[13] having completed 58.66% of its main sequence lifetime.[1]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 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.
  2. ↑ 2.0 2.1 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. ISSN 0004-6361. Bibcode: 2000A&A...355L..27H. 
  3. ↑ 3.0 3.1 Houk, Nancy (1978). Michigan catalogue of two-dimensional spectral types for the HD stars: Declinations −53° to −40°. 2. Bibcode: 1978mcts.book.....H. 
  4. ↑ 4.0 4.1 Alexander, J. B. (1972). "UBV observations of the RR Lyrae variable HD 176387 (MT Telescopii).". Royal Greenwich Observatory Bulletins 174: 107. Bibcode: 1972RGOB..174..107A. 
  5. ↑ 5.0 5.1 Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35,495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. ISSN 1063-7737. Bibcode: 2006AstL...32..759G. 
  6. ↑ 6.0 6.1 Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331–346. doi:10.1134/S1063773712050015. ISSN 1063-7737. Bibcode: 2012AstL...38..331A. 
  7. ↑ 7.0 7.1 7.2 7.3 Stassun, Keivan G. et al. (9 September 2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal 158 (4): 138. doi:10.3847/1538-3881/ab3467. Bibcode: 2019AJ....158..138S. 
  8. ↑ 8.0 8.1 Kervella, P.; Thévenin, F.; Di Folco, E.; Ségransan, D. (October 2004). "The angular sizes of dwarf stars and subgiants. Surface brightness relations calibrated by interferometry". Astronomy & Astrophysics 426 (1): 297–307. doi:10.1051/0004-6361:20035930. ISSN 0004-6361. Bibcode: 2004A&A...426..297K. 
  9. ↑ Anders, F. et al. (August 2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy & Astrophysics 628: A94. doi:10.1051/0004-6361/201935765. ISSN 0004-6361. Bibcode: 2019A&A...628A..94A. 
  10. ↑ 10.0 10.1 Gontcharov, G. A. (December 2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters 38 (12): 771–782. doi:10.1134/S1063773712120031. ISSN 1063-7737. Bibcode: 2012AstL...38..771G. 
  11. ↑ Oelkers, Ryan J.; Rodriguez, Joseph E.; Stassun, Keivan G.; Pepper, Joshua; Somers, Garrett; Kafka, Stella; Stevens, Daniel J.; Beatty, Thomas G. et al. (2018). "Variability Properties of Four Million Sources in the TESS Input Catalog Observed with the Kilodegree Extremely Little Telescope Survey". The Astronomical Journal 155 (1): 39. doi:10.3847/1538-3881/aa9bf4. Bibcode: 2018AJ....155...39O. 
  12. ↑ Andersen, J.; Nordstrom, B. (1983). "Radial velocities of bright southern stars. I - 139 B-type HR and FK stars". Astronomy and Astrophysics Supplement Series 52: 471–482. Bibcode: 1983A&AS...52..471A. 
  13. ↑ 13.0 13.1 Gontcharov, G. A. (November 2012). "Spatial distribution and kinematics of OB stars". Astronomy Letters 38 (11): 694–706. doi:10.1134/S1063773712110035. ISSN 1063-7737. Bibcode: 2012AstL...38..694G. 
  14. ↑ "HD 177406". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+177406. 
  15. ↑ Eggleton, P. P.; Tokovinin, A. A. (11 September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society 389 (2): 869–879. doi:10.1111/j.1365-2966.2008.13596.x. ISSN 0035-8711. Bibcode: 2008MNRAS.389..869E. 
  16. ↑ Gontcharov, George A.; Mosenkov, Aleksandr V. (28 September 2017). "Verifying reddening and extinction for Gaia DR1 TGAS main sequence stars". Monthly Notices of the Royal Astronomical Society 472 (4): 3805–3820. doi:10.1093/mnras/stx2219. ISSN 0035-8711. Bibcode: 2017MNRAS.472.3805G. 
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