HD 145377

HD 145377 is a star in the southern constellation Scorpius. It has an apparent visual magnitude of 8.10[2] and can be viewed with a small telescope. The star is located at a distance of 175 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +11.6.[5] The absolute magnitude of this star is 4.31,[6] indicating it would be visible to the naked eye if it were at a distance of 10 parsecs.

HD 145377
Observation data
Epoch J2000      Equinox J2000
Constellation Scorpius
Right ascension 16h 11m 36.44650s[1]
Declination −27° 04′ 41.4338″[1]
Apparent magnitude (V) 8.10[2]
Characteristics
Spectral type G3V[3]
Apparent magnitude (B) 8.73[2]
Apparent magnitude (J) 7.014±0.018[4]
Apparent magnitude (H) 6.797±0.040[4]
Apparent magnitude (K) 6.706±0.018[4]
B−V color index 0.63[2]
Astrometry
Radial velocity (Rv)+11.610±0.0011[5] km/s
Proper motion (μ) RA: +21.786[1] mas/yr
Dec.: +13.039[1] mas/yr
Parallax (π)18.6669 ± 0.0498[1] mas
Distance174.7 ± 0.5 ly
(53.6 ± 0.1 pc)
Absolute magnitude (MV)4.31[6]
Details
Mass1.129±0.022[7] M☉
Radius1.05±0.02 R☉[8]
1.12±0.03[9] R☉
Luminosity1.56±0.17 L☉[6]
1.43±0.04[9] L☉
Surface gravity (log g)4.38±0.03[9] cgs
Temperature6,046±15[6] K
Metallicity [Fe/H]0.12±0.01[6] dex
Rotation12 days[6]
Rotational velocity (v sin i)3.85[6] km/s
Age0.857±0.732[6] Gyr[7]
2.90±1.20[9] Gyr
Other designations
CD−26°11249, HD 145377, HIP 79346, SAO 184208, PPM 265238, GSC 06801-00585, 2MASS J16113644-2704414[10]
Database references
SIMBADdata
Exoplanet Archivedata
Extrasolar Planets
Encyclopaedia		data

This is an ordinary G-type main-sequence star with a stellar classification of G3V,[3] which indicates it is undergoing core hydrogen fusion. It is 5–12% larger and 13% more massive than the Sun. It may be younger than the Sun, with age estimates in the range of 1–3 billion years. The star is spinning with a projected rotational velocity of 3.85 km/s, giving it a rotation period of ~12 days.[6] The abundance of elements more massive than helium – what astronomers term the star's metallicity – is ~31% higher than in the Sun.[6] The star is radiating around 43% to 56% of the luminosity of the Sun from its photosphere at an effective temperature of 6,046 K.[6]

Planetary system

In October 2008 an extrasolar planet, HD 145377 b, was reported to be orbiting this star. This object was detected using the radial velocity method by search programs conducted using the HARPS spectrograph. It is a super-Jupiter in an eccentric orbit with a period of 104 days.[6]

The HD 145377 planetary system[6]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥5.76 ± 0.1 MJ 0.45 ± 0.004 103.95 ± 0.13 0.307 ± 0.017 — —

See also
  • List of extrasolar planets

References
  1. 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. Høg, E.; et al. (2000). The Tycho-2 catalogue of the 2.5 million brightest stars. Astronomy and Astrophysics. 355. pp. L27. Bibcode:2000A&A...355L..27H. doi:10.1888/0333750888/2862. ISBN 978-0333750889.
  3. Houk, Nancy (1979). Michigan catalogue of two-dimensional spectral types for the HD stars. 3. Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan. Bibcode:1982mcts.book.....H.
  4. Cutri, R. M.; et al. (June 2003). "2MASS All-Sky Catalog of Point Sources". VizieR On-line Data Catalog: II/246. Bibcode:2003yCat.2246....0C.
  5. Soubiran, C.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv:1804.09370. Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795.
  6. Moutou, C.; et al. (2009). "The HARPS search for southern extra-solar planets XVII. Six long-period giant planets around BD -17 0063, HD 20868, HD 73267, HD 131664, HD 145377, HD 153950". Astronomy and Astrophysics. 496 (2): 513–519. arXiv:0810.4662. Bibcode:2009A&A...496..513M. doi:10.1051/0004-6361:200810941.
  7. 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. A78.
  8. Stassun, Keivan G.; et al. (March 2017). "Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes". The Astronomical Journal. 153 (3): 20. arXiv:1609.04389. Bibcode:2017AJ....153..136S. doi:10.3847/1538-3881/aa5df3. S2CID 119219062. 136.
  9. Bonfanti, A.; Ortolani, S.; Nascimbeni, V. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics. 585: A5, 14 pp. arXiv:1511.01744. Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297. S2CID 53971692.
  10. "HD 145377". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2015-12-02.

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