HD 147513

Last updated
HD 147513
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Scorpius
Right ascension 16h 24m 01.28927s [1]
Declination −39° 11′ 34.7121″ [1]
Apparent magnitude  (V)5.38 [2]
Characteristics
Spectral type G1VH-04 [3]
U−B color index +0.00 [2]
B−V color index +0.62 [2]
Variable type suspected [4]
Astrometry
Radial velocity (Rv)+12.6 [5]  km/s
Proper motion (μ)RA: 71.89 [1]   mas/yr
Dec.: 5.26 [1]   mas/yr
Parallax (π)78.26 ± 0.37  mas [1]
Distance 41.7 ± 0.2  ly
(12.78 ± 0.06  pc)
Absolute magnitude  (MV)4.82 [6]
Details
Mass 1.11 [6]   M☉
Radius 1.0 [7]   R☉
Luminosity 0.98 [6]   L☉
Surface gravity (log g)4.50 [8]   cgs
Temperature 5,855 [8]   K
Metallicity [Fe/H]0.03 [8]   dex
Rotation 4.7 [6]  days
Rotational velocity (v sin i)0.32 [9]  km/s
Age 400 [10]   Myr
Other designations
62 G. Sco, CD −38° 10983, CPD −38° 6407, FK5  3295, GC 22030, Gl  620.1, HIP  80337, HR  6094, SAO  207622, Wo  9559. [11]
Database references
SIMBAD data
ARICNS data

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". [12] With an apparent magnitude of 5.38, [2] 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. [1]

Contents

Properties

This is a Sun-like main sequence star with a stellar classification of G1VH-04. [3] It has about 11% greater mass than the Sun, and is considered young with an estimated age of 400 million years. [10] 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. [13] HD 147513 is suspected of being a variable star. [14]

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. [13]

Planetary system

In 2002, the Geneva Extrasolar Planet Search Team announced the discovery of an extrasolar planet orbiting the star. [6] 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. [15]

The HD 147513 planetary system [6]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b >1.21  MJ 1.32528.4 ± 6.30.26 ± 0.05——

See also

Related Research Articles

HD 83443 is an orange dwarf star approximately 134 light-years away in the constellation of Vela. As of 2000, at least one extrasolar planet has been confirmed to be orbiting the star. The star HD 83443 is named Kalausi. The name was selected in the NameExoWorlds campaign by Kenya, during the 100th anniversary of the IAU. The word Kalausi means a very strong whirling column of wind in the Dholuo language.

HD 27894 is a 9th magnitude star located approximately 143 light years away in the constellation of Reticulum. It is an orange dwarf, a type dimmer and cooler than the Sun.

<span class="mw-page-title-main">HD 192263</span> Star in the constellation Aquila

HD 192263 is an 8th magnitude star about 64 light years away in the constellation of Aquila. The spectral type of the star is K2V, meaning that it is an orange dwarf, a type of star somewhat cooler and less luminous than the Sun. It is not visible to the unaided eye, but with good binoculars or small telescope it should be easy to spot.

HD 69830 is a yellow dwarf star located 41.0 light-years away in the constellation of Puppis. In 2005, the Spitzer Space Telescope discovered a narrow ring of warm debris orbiting the star. The debris ring contains substantially more dust than the Solar System's asteroid belt. In 2006, three extrasolar planets with minimum masses comparable to Neptune were confirmed in orbit around the star, located interior to the debris ring.

HD 28185 is a yellow dwarf star similar to the Sun located 128 light-years away from Earth in the constellation Eridanus. The designation HD 28185 refers to its entry in the Henry Draper catalogue. The star is known to possess one long-period extrasolar planet.

Chi Scorpii, Latinized from χ Scorpii, is a single star in the zodiac constellation of Scorpius. It has an orange hue and can be faintly seen with the naked eye with an apparent visual magnitude of 5.22. Based upon parallax measurements, this star is around 409 light years from the Sun. The star is drifting closer with a radial velocity of −23.6 km/s.

<span class="mw-page-title-main">HD 219134</span> Star in the constellation Cassiopeia

HD 219134 is a main-sequence star in the constellation of Cassiopeia. It is smaller and less luminous than the Sun, with a spectral class of K3V, which makes it an orange-hued star. HD 219134 is relatively close to our system, with an estimated distance of 21.34 light years. This star is close to the limit of apparent magnitude that can still be seen by the unaided eye. The limit is considered to be magnitude 6 for most observers. This star has a magnitude 9.4 optical companion at an angular separation of 106.6 arcseconds.

HD 1237 is a binary star system approximately 57 light-years away in the constellation of Hydrus.

HD 4308 is a single star in the southern constellation of Tucana. It has a yellow hue and is a challenge to view with the naked eye even under good seeing conditions, having an apparent visual magnitude of 6.54. This object is located at a distance of 72 light years, as determined from parallax measurements. It is a population II star and is considered to be a member of the thick disk. The star is receding from the Sun with a radial velocity of +95 km/s.

94 Ceti is a trinary star system approximately 73 light-years away in the constellation Cetus.

Gliese 86 is a K-type main-sequence star approximately 35 light-years away in the constellation of Eridanus. It has been confirmed that a white dwarf orbits the primary star. In 1998 the European Southern Observatory announced that an extrasolar planet was orbiting the star.

HD 176051 is a spectroscopic binary star system approximately 49 light years away from Earth in the constellation Lyra. The pair orbit with a period of 22,423 days and an eccentricity of 0.25. Compared to the Sun, they have a somewhat lower proportion of elements more massive than helium. Their individual masses are estimated at 1.07 and 0.71 solar masses (M☉). The system is moving closer to the Sun with a radial velocity of −47 km/s and will reach perihelion in about 269,000 years when it comes within roughly 17 ly (5.1 pc) of the Sun.

HD 213240 is a possible binary star system in the constellation Grus. It has an apparent visual magnitude of 6.81, which lies below the limit of visibility for normal human sight. The system is located at a distance of 133.5 light years from the Sun based on parallax. The primary has an absolute magnitude of 3.77.

<span class="mw-page-title-main">V538 Aurigae</span> Star in constellation Auriga

V538 Aurigae is a single star in the northern constellation of Auriga. With an apparent visual magnitude of 6.23, this star requires good dark sky conditions to view with the naked eye. It is located at a distance of 40.0 light-years (12.3 pc) from Sun based on parallax. The star is drifting further away with a radial velocity of 0.9 km/s. It is a member of the Local Association, and is most likely a thin disk star.

HD 60532 is a white (F-type) main sequence star located approximately 84 light-years away in the constellation of Puppis, taking its primary name from its Henry Draper Catalogue designation. It is calculated to be 1.44 times more massive than the Sun. The star is only 59% as old as the Sun and has metallicity of only 38% that of the Sun. In 2008, two extrasolar planets were discovered in orbit around it.

HD 6718 is a solar twin star in the equatorial constellation of Cetus. It has a yellow hue but is too faint to be viewed with the naked eye, having an apparent visual magnitude of 8.45. The distance to this object, as determined from parallax measurements, is 168 light years. It is drifting away from the Sun with a radial velocity of +35 km/s.

HIP 70849 is a star with two non-stellar companions in the southern constellation Lupus. It is a 10th magnitude star, making it too faint to be visible to the naked eye. The system is located at a distance of 78.7 light-years from the Sun based on parallax measurements.

HD 129445 is a G-type star found in the Circinus constellation located 219 light-years away from the Sun based on parallax. It is invisible to the naked eye with an apparent visual magnitude of 8.80. The star was observed by the Magellan Planet Search Program due to its absolute visual magnitude and high metallicity. The Magellan program conducted 17 doppler velocity measurements, which spans a full orbital period. The results led the program to detect a planet dubbed HD 129445 b. In 2023, the inclination and true mass of HD 129445 b were determined via astrometry.

Gliese 251, also known as HIP 33226 or HD 265866, is a star located about 18 light years away from the Solar System. Located in the constellation of Gemini, it is the nearest star in this constellation. It is located near the boundary with Auriga, 49 arcminutes away from the bright star Theta Geminorum; due to its apparent magnitude of +9.89 it cannot be observed with the naked eye. The closest star to Gliese 251 is QY Aurigae, which is located 3.5 light years away.

References

  1. 1 2 3 4 5 6 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.
  2. 1 2 3 4 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
  3. 1 2 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.
  4. ↑ 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.
  5. ↑ 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.
  6. 1 2 3 4 5 6 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.
  7. ↑ Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics (Third ed.), 367 (2): 521–524, arXiv: astro-ph/0012289 , Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID   425754.
  8. 1 2 3 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.
  9. ↑ 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.
  10. 1 2 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.
  11. ↑ "HR 6094". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2015-05-22.{{cite web}}: CS1 maint: postscript (link)
  12. ↑ Piazzi, G., (ed.) the Palermo Catalogue, 1814.
  13. 1 2 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 .
  14. ↑ NSV 7680 -- Variable Star - SIMBAD entry
  15. ↑ 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
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.