Astronomy:HD 128294

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Short description: Blue giant in the constellation Apus
HD 128294
Observation data
Epoch J2000.0   Equinox (celestial coordinates)
Constellation Apus
Right ascension  14h 41m 59.70978s[1]
Declination −77° 00′ 41.2260″[1]
Apparent magnitude (V) 6.34±0.01[2]
Characteristics
Evolutionary stage main sequence[1]
Spectral type B9 III[3]
B−V color index −0.027±0.002[4]
Astrometry
Radial velocity (Rv)8.94±2.29[1] km/s
Proper motion (μ) RA: −21.428[1] mas/yr
Dec.: −12.249[1] mas/yr
Parallax (π)5.2747 ± 0.0603[1] mas
Distance618 ± 7 ly
(190 ± 2 pc)
Absolute magnitude (MV)+0.07[4]
Details
Mass2.66+0.47−0.25[5] M
Radius3.62±0.11[5] R
Luminosity145+20−31[1] L
Surface gravity (log g)3.75+0.09−0.04[5] cgs
Temperature10,336+158−296[5] K
Metallicity [Fe/H]−0.09[6] dex
Age286[7] Myr
Other designations
CD−76°655, CPD−76°848, GC 19736, HD 128294, HIP 71870, SAO 257182[8]
Database references
SIMBADdata

HD 128294 is a solitary, bluish-white hued star located in the southern circumpolar constellation Apus. It has an apparent magnitude of 6.34,[2] placing it near the limit for naked eye visibility, even under ideal conditions. Gaia DR3 parallax measurements imply a distance of 618 light-years.[1] At its current distance, HD 128294's brightness is heavily diminished by 0.43 magnitudes due to interstellar extinction[9] and it has an absolute magnitude of +0.07.[4]

HD 128294 has a stellar classification of B9 III,[3] indicating that it is an evolved blue giant. At the age of 286 million years,[7] the object has completed 71.9% of its main sequence lifetime according to Gaia DR3 models.[1] It has 2.66 times the mass of the Sun and a slightly enlarged radius 3.62 times that of the Sun's.[5] It radiates 145 times the luminosity of the Sun[1] from its photosphere at an effective temperature of 10,336 K.[5] According to astrophysical parameters based on the Gaia passband, HD 128294 has an iron abundance 81.3% that of the Sun's ([Fe/H) = −0.09),[6] making it slightly metal deficient.

References

  1. 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 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. Bibcode2000A&A...355L..27H. 
  3. 3.0 3.1 Houk, N.; Cowley, A. P. (1975). University of Michigan Catalogue of two-dimensional spectral types for the HD stars: Declinations −90° to −53°. 1. Bibcode1975mcts.book.....H. 
  4. 4.0 4.1 4.2 Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331–346. doi:10.1134/S1063773712050015. ISSN 1063-7737. Bibcode2012AstL...38..331A. 
  5. 5.0 5.1 5.2 5.3 5.4 5.5 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. Bibcode2019AJ....158..138S. 
  6. 6.0 6.1 Anders, F. et al. (February 2022). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia EDR3 stars brighter than G = 18.5". Astronomy & Astrophysics 658: A91. doi:10.1051/0004-6361/202142369. ISSN 0004-6361. Bibcode2022A&A...658A..91A. 
  7. 7.0 7.1 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. Bibcode2012AstL...38..694G. 
  8. "HD 128294". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+128294. 
  9. 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. Bibcode2017MNRAS.472.3805G. 
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