HD 147513

In today's world, HD 147513 has become a topic of great relevance and interest to a wide range of people. Whether due to its impact on society, its importance in the workplace or its relevance in history, HD 147513 has captured the attention of many and has generated intense debate in various circles. In this article, we will explore the different aspects of HD 147513, analyzing its influence in the past, present and future. From its origins to its possible long-term implications, we will delve into the world of HD 147513 to better understand its scope and meaning.

HD 147513
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Scorpius[1]
Right ascension 16h 24m 01.28927s[2]
Declination −39° 11′ 34.7121″[2]
Apparent magnitude (V) 5.38[3]
Characteristics
Spectral type G1V CH-04[4]
U−B color index +0.00[3]
B−V color index +0.62[3]
Variable type suspected[5]
Astrometry
Radial velocity (Rv)+12.6[6] km/s
Proper motion (μ) RA: 71.89[2] mas/yr
Dec.: 5.26[2] mas/yr
Parallax (π)78.26±0.37 mas[2]
Distance41.7 ± 0.2 ly
(12.78 ± 0.06 pc)
Absolute magnitude (MV)4.82[7]
Details
Mass1.11[7] M☉
Radius1.0[8] R☉
Luminosity0.98[7] L☉
Surface gravity (log g)4.50[9] cgs
Temperature5,855[9] K
Metallicity 0.03[9] dex
Rotation4.7[7] days
Rotational velocity (v sin i)0.32[10] km/s
Age400[11] Myr
Other designations
62 G. Sco, CD−38°10983, CPD−38°6407, FK5 3295, GC 22030, Gl 620.1, GJ 9559, HIP 80337, HR 6094, SAO 207622, Wo 9559[12]
Database references
SIMBADdata
ARICNSdata

HD 147513 (62 G. Scorpii) is a star in the southern constellation of Scorpius. It was first catalogued by Italian astronomer Piazzi in his star catalogue as "XVI 55".[13] With an apparent magnitude of 5.38,[3] according to the Bortle scale it is visible to the naked eye from suburban skies. Based upon stellar parallax measurements by the Hipparcos spacecraft, HD 147513 lies some 42 light years from the Sun.[2]

Properties

This is a Sun-like main sequence star with a stellar classification of G1V CH-04.[4] It has about 11% greater mass than the Sun, and is considered young with an estimated age of 400 million years.[11] As such, it has a similar luminosity to the Sun despite being more massive. Although the abundance of elements is similar to the Sun, it is a Barium star that is overabundant in elements produced through the s-process.[14] HD 147513 is suspected of being a variable star.[15]

HD 147513 is a member of the Ursa Major moving group that share a common proper motion through space. It has a nearby co-moving companion: a DA-class white dwarf located some 5,360 AU distant, where an AU is the average separation of the Earth from the Sun. At one time the pair may have been members of a multiple star system. The progenitor of the white dwarf may have been a closer companion, and while passing through the asymptotic giant branch stage of its evolution, could have transferred matter onto HD 147513 and contaminated this star's photosphere.[14]

Planetary system

In 2002, the Geneva Extrasolar Planet Search Team announced the discovery of an extrasolar planet orbiting the star.[7] Based upon the orbital elements, most of this gas giant's orbit lies within the habitable zone (HZ) of the host star; it only passes outside this region at apogee. As such, it is unlikely that a terrestrial planet could have a stable orbit within the HZ unless it moves in a synchronized fashion with the gas giant. Numerical simulations suggest that such a planet could orbit within the L4 or L5 Lagrangian points of the gas giant.[16]

The HD 147513 planetary system[7]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b >1.21 MJ 1.32 528.4 ± 6.3 0.26 ± 0.05 — —

See also

References

  1. ^ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015.
  2. ^ a b c d e f van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  3. ^ a b c d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
  4. ^ a b Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
  5. ^ Kukarkin, B. V.; et al. (1981), "Nachrichtenblatt der Vereinigung der Sternfreunde e.V. (Catalogue of suspected variable stars)", Nachrichtenblatt der Vereinigung der Sternfreunde, Moscow: Academy of Sciences USSR Shternberg, Bibcode:1981NVS...C......0K.
  6. ^ Nordström, B.; et al. (2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ~14000 F and G dwarfs", Publications of the Astronomical Society of Australia, 21 (2): 129–133, arXiv:0811.3982, Bibcode:2004PASA...21..129N, doi:10.1071/AS04013, S2CID 123457673.
  7. ^ a b c d e f Mayor, M.; et al. (2004). "The CORALIE survey for southern extra-solar planets XII. Orbital solutions for 16 extra-solar planets discovered with CORALIE". Astronomy and Astrophysics. 415 (1): 391–402. arXiv:astro-ph/0310316. Bibcode:2004A&A...415..391M. doi:10.1051/0004-6361:20034250. S2CID 5233877.
  8. ^ Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics, 367 (2) (Third ed.): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
  9. ^ a b c Ramírez, I.; et al. (February 2013), "Oxygen abundances in nearby FGK stars and the galactic chemical evolution of the local disk and halo", The Astrophysical Journal, 764 (1): 78, arXiv:1301.1582, Bibcode:2013ApJ...764...78R, doi:10.1088/0004-637X/764/1/78, S2CID 118751608.
  10. ^ Martínez-Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter" (PDF), Astronomy and Astrophysics, 520: A79, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725, S2CID 43455849, archived from the original (PDF) on 2017-09-22, retrieved 2018-11-04.
  11. ^ a b Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008). "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics". The Astrophysical Journal. 687 (2): 1264–1293. arXiv:0807.1686. Bibcode:2008ApJ...687.1264M. doi:10.1086/591785. S2CID 27151456.
  12. ^ "HR 6094", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2015-05-22.
  13. ^ Piazzi, G., (ed.) the Palermo Catalogue, 1814.
  14. ^ a b Porto de Mello, G. F.; da Silva, L. (1997). "HR 6094: A Young, Solar-Type, Solar-Metallicity Barium Dwarf Star". Astrophysical Journal Letters. 476 (2): L89. Bibcode:1997ApJ...476L..89P. doi:10.1086/310504.
  15. ^ NSV 7680 -- Variable Star - SIMBAD entry
  16. ^ Funk, B.; et al. (July 2012), "On the stability of possible Trojan planets in the habitable zone: an application to the systems HD 147513 and HD 210277", Monthly Notices of the Royal Astronomical Society, 423 (4): 3074–3082, Bibcode:2012MNRAS.423.3074F, doi:10.1111/j.1365-2966.2012.21121.x