HD 126053

Last updated
HD 126053
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Virgo
Right ascension 14h 23m 15.285s [1]
Declination +01° 14′ 29.64″ [1]
Apparent magnitude  (V)6.25 [2]
Characteristics
HD 126053 A
Evolutionary stage Main sequence
Spectral type G1 V [3]
U−B color index +0.09 [4]
B−V color index 0.639 [2]
HD 126053 B
Evolutionary stage Brown dwarf
Spectral type T8 [5]
Astrometry
Radial velocity (Rv)−19.17±0.06 [2]  km/s
Proper motion (μ)RA: 223.531  mas/yr [1]
Dec.: −478.275  mas/yr [1]
Parallax (π)57.2706 ± 0.0375  mas [1]
Distance 56.95 ± 0.04  ly
(17.46 ± 0.01  pc)
Details
HD 126053 A
Mass 0.89 [6]   M☉
Radius 0.93 [7]   R☉
Luminosity 0.83 [6]   L☉
Luminosity (bolometric)0.812 [8]   L☉
Surface gravity (log g)4.57 [9]   cgs
Temperature 5,722 [9]   K
Metallicity [Fe/H]−0.28 [9]   dex
Rotation 22 d [10]
Rotational velocity (v sin i)3.08 [3]  km/s
Age 5.490 [11]   Gyr
HD 126053 B
Mass 0.019-0.047 [5]   M☉
Radius 0.080-0.099 [5]   R☉
Temperature 680±55 [5]   K
Metallicity [Fe/H]−0.38±0.06 [5]   dex
Other designations
BD+01°2920, GJ  547, HD  126053, HIP  70319, HR  5384, SAO  120424 [12]
Database references
SIMBAD data

HD 126053 is the Henry Draper Catalogue designation for a star in the equatorial constellation of Virgo. It has an apparent magnitude of 6.25, [2] which means it is faintly visible to the naked eye. According to the Bortle scale, it requires dark suburban or rural skies to view. Parallax measurements made by the Hipparcos spacecraft provide an estimated distance of 57  light years to this star. [1] It is drifting closer with a heliocentric radial velocity of −19.2 km/s. [2]

This star is considered a solar analog—meaning that it is photometrically analogous to the Sun. [6] The physical properties of this star are similar to the Sun, although it is metal poor. [5] Like the Sun, it has a magnetic activity cycle. It shares a common proper motion through space with the spectroscopic binary star system HD 122742, and in the past the three may have formed a triple star system. In the Bright Star Catalogue, it was noted as having an infrared excess. This may have been accreted from the HD 122742 system when the three stars were closer to each other. [13]

In 2012, a brown dwarf was discovered orbiting this star at a distance of 2630 AU. [5]

Related Research Articles

Pi Serpentis, Latinized from π Serpentis, is a solitary white-hued star in the constellation Serpens, located in its head, Serpens Caput. Based upon an annual parallax shift of 18.22 mas as seen from Earth, it is located around 179 light years from the Sun. It is visible to the naked eye with an apparent visual magnitude of 4.82.

HD 211415 is a double star in the constellation Grus. With an apparent visual magnitude of 5.33, it is visible to the naked eye. The annual parallax shift is 72.54 mas, which yields a distance estimate of 45 light years. It has a relatively high proper motion, traversing the celestial sphere at the rate of 93.4 mas per year, and is moving closer to the Sun with a radial velocity of −13 km/s.

HD 4628 is a main sequence star in the equatorial constellation of Pisces. It has a spectral classification of K2.5 V and an effective temperature of 5,055 K, giving it an orange-red hue with a slightly smaller mass and girth than the Sun. HD 4628 lies at a distance of approximately 24.3 light years from the Sun based on parallax. The apparent magnitude of 5.7 is just sufficient for this star to be viewed with the unaided eye. The star appears to be slightly older than the Sun—approximately 5.4 billion years in age. The surface activity is low and, based upon the detection of UV emission, it may have a relatively cool corona with a temperature of one million K.

HD 49878 is a single star in the northern circumpolar constellation of Camelopardalis. It has an orange hue and is faintly visible to the naked eye with an apparent visual magnitude of +4.55. The star is located at a distance of approximately 184 light years from the Sun, as determined from its parallax. It is drifting closer with a radial velocity of −29.5 km/s. The star has been listed as a candidate member of the Wolf 630 moving group, but is most likely a field star.

HR 4458 is a binary star system in the equatorial constellation of Hydra. It has the Gould designation 289 G. Hydrae; HR 4458 is the Bright Star Catalogue designation. At a distance of 31.13 light years, it is the closest star system to the Solar System within this constellation. This object is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.97. It is moving closer to the Earth with a heliocentric radial velocity of −22 km/s.

<span class="mw-page-title-main">HD 17925</span> Star in the constellation Eridanus

HD 17925 is a variable star in the equatorial constellation of Eridanus. It has the Gould designation 32 G. Eridani and the variable star designation EP Eri. The star has a yellow-orange hue and is dimly visible to the naked eye in good seeing conditions with an apparent visual magnitude that varies from 6.03 down to 6.08. It is located nearby at a distance of 34 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +18 km/s. It is a likely member of the Local Association of nearby, co-moving stars. The spectrum shows a strong abundance of lithium, indicating that it is young star. This likely makes its point of origin the nearby Scorpio–Centaurus Complex.

HR 6806 or HD 166620 is a solitary, orange, main sequence, and Sun-like star located thirty-six light-years away, in the constellation Hercules. The star is smaller than the Sun, with around 79% of the solar mass and radius, and 35% of the solar luminosity. It appears to be rotating slowly with an estimated period of 42 days. In 1988, it was noticed that the star had an inactive chromosphere, with a surface magnetic field strength of only 1,500 G. From 1990 activity in the chromosphere increased, inline with a 16 year stellar cycle previously observed. But, sometime after 1994 chromospheric activity greatly reduced, and has stayed flat for more than 16 years. As of 2022, the star appears to have entered the equivalent of a Maunder minimum. The star is around six billion years of age.

HD 125072 is a star in the southern constellation of Centaurus. It is a challenge to view with the naked eye, having an apparent visual magnitude of 6.637. The star is located at a distance of 38.6 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −14.9 km/s. The components of the space velocity for this star are U=−18.5, V=−6.9 and W=−26.9 km/s.

<span class="mw-page-title-main">V1291 Aquilae</span> Variable star in the constellation Aquila

V1291 Aquilae is a single star in the equatorial constellation of Aquila. It has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude that fluctuates around 5.65. Based on parallax measurements, it is located at a distance of approximately 278 light years from the Sun. The star it is drifting closer with a radial velocity of −22 km/s.

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

IQ Aurigae is a single, variable star in the northern constellation of Auriga. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude that fluctuates around 5.38. The star is located at a distance of about 460 light-years from the Sun based on parallax and is drifting further away with a radial velocity of +28.6 km/s.

<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 127304 is a double star in the northern constellation of Boötes. The brighter component is a sixth magnitude A-type main sequence star with a stellar classification of A0Vs It has a faint magnitude 10.62 companion at an angular separation of 25.6″ along a position angle of 256°.

<span class="mw-page-title-main">Chi Ceti</span> Double star in the constellation Cetus

Chi Ceti , is the Bayer designation for a double star in the equatorial constellation of Cetus. They appear to be common proper motion companions, sharing a similar motion through space. The brighter component, HD 11171, is visible to the naked eye with an apparent visual magnitude of 4.66, while the fainter companion, HD 11131, is magnitude 6.75. Both lie at roughly the same distance, with the brighter component lying at an estimated distance of 75.6 light years from the Sun based upon an annual parallax shift of 43.13 mass.

<span class="mw-page-title-main">Epsilon Crateris</span> Solitary star in the constellation Crater

Epsilon Crateris is a solitary star in the southern constellation of Crater. Visible to the naked eye, it has an apparent visual magnitude of 4.84. It is located in the sky above Beta Crateris, and slightly to the left, or east, marking the lower right edge of the rim of the bowl and is somewhat closer to Theta Crateris, which is further east at the top of the bowl. With an annual parallax shift of 8.67 mas as seen from the Earth, its estimated distance is around 376 light years from the Sun.

Mu2 Octantis (μ2 Oct) is a binary star system of two G-type main-sequence stars. It shares the designation μ with μ1 Octantis, from which it is separated by 50 arcminutes.

HR 4699 is a single star in the southern constellation of Corvus. It is orange in hue and is dimly visible to the naked eye with an apparent visual magnitude of +5.14. This star is located at a distance of approximately 201 light years from the Sun based on parallax. It is drifting further away with a radial velocity of +14 km/s, after come to within 45.1 light-years some four million years ago.

Phi Phoenicis, Latinized from φ Phoenicis, is a binary star system in the southern constellation of Phoenix. It is faintly visible to the naked eye with an apparent visual magnitude of 5.1. Based upon an annual parallax shift of 10.185 mas as seen from Earth, it is located approximately 320 light years from the Sun. It is moving away with a heliocentric radial velocity of 10.4 km/s.

HD 33266 is a solitary star in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 6.17, making it faintly visible to the naked eye. Located 481 light years away, it is approaching the Sun with a heliocentric radial velocity of −4.4 km/s.

HR 2131 is a solitary star in the southern constellation Columba. It has an apparent magnitude of 5.52, allowing it to be faintly seen with the naked eye. The object is located at a distance of 670 light years but is receding with a heliocentric radial velocity of 19 km/s.

HD 46815 is a solitary star in the southern constellation Columba. It is faintly visible to the naked eye with an apparent magnitude of 5.4 and is estimated to be 408 light years away. However, it is receding with a heliocentric radial velocity of 32.2 km/s.

References

  1. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 3 4 5 Soubiran, C.; et al. (April 2013), "The catalogue of radial velocity standard stars for Gaia. I. Pre-launch release", Astronomy & Astrophysics, 552: 11, arXiv: 1302.1905 , Bibcode:2013A&A...552A..64S, doi:10.1051/0004-6361/201220927, S2CID   56094559, A64.
  3. 1 2 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.
  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.
  5. 1 2 3 4 5 6 7 Pinfield, D. J.; et al. (May 2012), "Discovery of the benchmark metal-poor T8 dwarf BD +01° 2920B", Monthly Notices of the Royal Astronomical Society , 422 (3): 1922–1932, arXiv: 1201.3243 , Bibcode:2012MNRAS.422.1922P, doi:10.1111/j.1365-2966.2012.20549.x, S2CID   6257539.
  6. 1 2 3 Do Nascimento, J. D.; et al. (September 2010), "Rotation and lithium abundance of solar-analog stars. Theoretical analysis of observations", Astronomy and Astrophysics, 519: 9, arXiv: 1006.3861 , Bibcode:2010A&A...519A.101D, doi:10.1051/0004-6361/200811026, S2CID   56098215, A101.
  7. ↑ Pasinetti Fracassini, L. E.; et al. (2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics", Astronomy & Astrophysics, 367 (2): 521–24, arXiv: astro-ph/0012289 , Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID   425754.
  8. ↑ Eiroa, C.; et al. (July 2013), "DUst around NEarby Stars. The survey observational results", Astronomy & Astrophysics, 555: A11, arXiv: 1305.0155 , Bibcode:2013A&A...555A..11E, doi:10.1051/0004-6361/201321050, S2CID   377244.
  9. 1 2 3 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.
  10. ↑ Baliunas, S.; Sokoloff, D.; Soon, W. (1996), "Magnetic Field and Rotation in Lower Main-Sequence Stars: an Empirical Time-dependent Magnetic Bode's Relation?", Astrophysical Journal Letters , 457 (2): L99, Bibcode:1996ApJ...457L..99B, doi: 10.1086/309891 .
  11. ↑ Vican, Laura (June 2012), "Age Determination for 346 Nearby Stars in the Herschel DEBRIS Survey", The Astronomical Journal, 143 (6): 135, arXiv: 1203.1966 , Bibcode:2012AJ....143..135V, doi:10.1088/0004-6256/143/6/135, S2CID   118539505.
  12. ↑ "HD 126053". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2015-11-13.{{cite web}}: CS1 maint: postscript (link)
  13. ↑ Frisch, P. C. (April 1993), "G-star astropauses - A test for interstellar pressure", Astrophysical Journal, Part 1, 407 (1): 198–206, Bibcode:1993ApJ...407..198F, doi:10.1086/172505.
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