HD 10307

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HD 10307
Andromeda constellation map.svg
Red circle.svg
Location of HD 10307 (circled)
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Andromeda
Right ascension 01h 41m 47.1431s [1]
Declination +42° 36′ 48.4435″ [1]
Apparent magnitude  (V)4.95 / 11 [2]
Characteristics
Spectral type G1.5 V + M V [3]
U−B color index 0.11 [4]
B−V color index 0.62 [4]
Astrometry
Radial velocity (Rv)3.1±0.12 [5]  km/s
Proper motion (μ)RA: 813.337±0.380 [1]   mas/yr
Dec.: −171.027±0.464 [1]   mas/yr
Parallax (π)79.08 ± 0.63  mas [6]
Distance 41.2 ± 0.3  ly
(12.6 ± 0.1  pc)
Absolute magnitude  (MV)4.43 [7]
Absolute bolometric
magnitude  (Mbol)		4.32±0.06 [8]
Orbit [6]
Period (P)19.542±0.014 yr
Semi-major axis (a)0.6104±0.0097″
Eccentricity (e)0.4367±0.0020
Inclination (i)100.36±0.89°
Longitude of the node (Ω)32.25±0.35°
Periastron epoch (T)2016.702±0.012
Argument of periastron (ω)
(secondary)		27.15±0.35°
Semi-amplitude (K1)
(primary)		2.7160±0.0072 km/s
Details [8]
HD 10307 A
Mass 0.95±0.11 [6]   M☉
Radius 1.14±0.04  R☉
Luminosity 1.44  L☉
Surface gravity (log g)4.3±0.1  cgs
Temperature 5,878±60  K
Metallicity [Fe/H]+0.00±0.06  dex
Rotational velocity (v sin i)1.5±1.0 km/s
Age 7.0 [9]   Gyr
HD 10307 B
Mass 0.254±0.019 [6]   M☉
Luminosity0.0013 [10]   L☉
Other designations
BD+41°328, GJ  67, HD  10307, HIP  7918, HR  483, SAO  37434, LHS  1284, YPC 350
Database references
SIMBAD HD 10307
ARICNS HD 10307 A
HD 10307 B

HD 10307 (HR 483) is a spectroscopic binary star in the constellation Andromeda. The primary is similar to the Sun in mass, temperature and metal content. It is situated about 42 light-years from Earth. Its companion, HR 483 B, is a little-studied red dwarf.

Contents

HD 10307 was identified in September 2003 by astrobiologist Margaret Turnbull from the University of Arizona in Tucson as one of the most promising nearby candidates for hosting life based on her analysis of the HabCat list of stars. [11]

System

HD 10307 in optical light HIP7918.jpg
HD 10307 in optical light

HR 483 is a binary located 42.6 ly away, in Andromeda. The two stars orbit one another elliptically (e=0.44), [12] approaching as close as 4.2 AU and receding to 10.5 AU, with a period of just under twenty years. [6]

HD 10307 A, the larger component, is a G-type main-sequence star similar to the Sun, only slightly brighter, hotter, larger, and older than the Sun—though with a slightly smaller mass. It has a low level of activity and is a candidate Maunder minimum analog. [13] HR 483 B, the smaller component, appears to be a red dwarf, with as little as thirty-eight percent the mass of the sun. [3] A debris disk has been detected in this system. [14]

The presence of a moderately close companion could disrupt the orbit of a hypothetical planet in HD 10307's habitable zone. However, the uncertainty of the orbital parameters makes it equally uncertain exactly where stable orbits would be in this system. [10]

METI message to HD 10307

There was a METI message sent to HD 10307. It was transmitted from Eurasia's largest radar, 70-meter Eupatoria Planetary Radar. The message was named Cosmic Call 2, it was sent on July 6, 2003, and it will arrive at HD 10307 in September 2044. [15]

Related Research Articles

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HD 75289 is a faint double star in the southern constellation of Vela. The primary component has a yellow hue and an apparent visual magnitude of 6.35. Under exceptionally good circumstances it might be visible to the unaided eye; however, usually binoculars are needed. The pair are located at a distance of 95 light years from the Sun based on parallax, and are drifting further away with a radial velocity of +10 km/s.

<span class="mw-page-title-main">Epsilon Reticuli</span> Star in the constellation Reticulum

Epsilon Reticuli, Latinized from ε Reticuli, is a double star approximately 60 light-years away in the southern constellation of Reticulum. The brighter member is visible to the naked eye with an apparent visual magnitude of 4.44. The primary component is an orange subgiant, while the secondary is a white dwarf. The two stars share a common motion through space and hence most likely form a binary star system. The brighter star should be easily visible without optical aid under dark skies in the southern hemisphere. In 2000, an extrasolar planet was confirmed to be orbiting the primary star in the system.

HD 202206 is a binary star system in the southern constellation of Capricornus. With an apparent visual magnitude of +8.1, it is too faint to be visible to the naked eye. It is located at a distance of 150 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +14.7 km/s.

HR 3220 is a binary star system in the southern constellation of Carina. It has the Bayer designation B Carinae; HR 3220 is the designation from the Bright Star Catalogue. It has a yellow-white hue and is visible to the naked eye with an apparent visual magnitude of 4.75. Based upon parallax measurements, it is located at a distance of 59 light years from the Sun. The system is drifting further away with a radial velocity of +24 km/s.

HD 222582 is a multiple star system in the equatorial constellation of Aquarius. It is invisible to the naked eye with an apparent visual magnitude of 7.7, but can be viewed with binoculars or a small telescope. The system is located at a distance of 137 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +12 km/s. It is located close enough to the ecliptic that it is subject to lunar occultations.

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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.

<span class="mw-page-title-main">V1054 Ophiuchi</span> Star system in the constellation Ophiuchus

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HD 83380 is an orange-hued star in the southern constellation of Antlia. It shines faintly with a apparent magnitude of 5.62 when viewed in ideal conditions. Parallax measurements place the object at distance of 312 light-years. It has a heliocentric radial velocity of −2.6 km/s, indicating that it is drifting towards the Solar System.

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HD 168009 is a star in the northern constellation of Lyra. It has an apparent visual magnitude of 6.3, placing it just above to below the normal limit of stars visible to the naked eye under good viewing conditions of 6-6.5. An annual parallax shift of 42.93 mas provides a distance estimate of 76 light years. It is moving closer to the Sun with a heliocentric radial velocity of −65 km/s. In about 328,000 years from now, the star will make its closest approach at a distance of around 17 ly (5.1 pc).

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<span class="mw-page-title-main">14 Trianguli</span> Star in the constellation Triangulum

14 Trianguli, also known as HD 15656, is a spectroscopic binary located in the northern constellation Triangulum. It has an apparent magnitude of 5.14, making it faintly visible to the naked eye in ideal conditions. Gaia DR3 parallax measurements place the system 433 light years away, and it is currently approaching the Solar System with a heliocentric radial velocity of −37 km/s. At its current distance, 14 Tri's brightness is diminished by 0.21 magnitude due to interstellar dust. It has an absolute magnitude of −0.46.

HD 72945 and HD 72946 form a co-moving star system in the northern constellation of Cancer. HD 72945 is a binary star that is dimly visible to the naked eye as a point of light with an apparent visual magnitude of 5.91. At an angular separation of 10.10″ is the fainter companion star HD 72946 at magnitude 7.25. It is being orbited by a brown dwarf. The system as a whole is located at a distance of approximately 84 light years from the Sun based on parallax measurements.

HD 10800, also known as HR 512 or Gliese 67.1, is a triple star located in the southern circumpolar constellation Octans. It has a combined apparent magnitude of 5.87, allowing it to be faintly seen with the naked eye. The system is relatively close at a distance of 88.1 light years but is drifting closer with a heliocentric radial velocity −1.1 km/s.

<span class="mw-page-title-main">HD 28204</span> Spectroscopic binary in the constellation Camelopardalis

HD 28204, also designated as HR 1401, is a spectroscopic binary located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.93, making it faintly visible to the naked eye under ideal conditions. Gaia DR3 parallax measurements imply a distance of 331 light-years and it is currently receding with a heliocentric radial velocity of 9 km/s. At its current distance, HD 28204's brightness is diminished by 0.18 magnitudes due to interstellar extinction and it has an absolute magnitude of +0.91.

References

  1. 1 2 3 4 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. ↑ "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Archived from the original on 2017-08-01. Retrieved 2017-05-21.
  3. 1 2 Belikov, A. N. (1995). "Stellar Mass Catalogue (SMAC). Preliminary version". Bulletin d'Information du Centre de Données Stellaires. 47: 9. Bibcode:1995BICDS..47....9B.
  4. 1 2 Database entry, Catalogue of Stellar Photometry in Johnson's 11-color system (2002 Ed.), J. R. Ducati, CDS ID II/237 Accessed on line 2018-12-05.
  5. ↑ Pourbaix, D.; et al. (September 2004), "SB9: The ninth catalogue of spectroscopic binary orbits", Astronomy and Astrophysics, 424 (2): 727–732, arXiv: astro-ph/0406573 , Bibcode:2004A&A...424..727P, doi:10.1051/0004-6361:20041213, S2CID   119387088.
  6. 1 2 3 4 5 Torres, Guillermo (2022). "Orbital solution and dynamical masses for the nearby binary system GJ 67 AB". Monthly Notices of the Royal Astronomical Society. 514 (4): 5183–5191. arXiv: 2206.10627 . Bibcode:2022MNRAS.514.5183T. doi:10.1093/mnras/stac1710.
  7. ↑ Holmberg, J.; et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv: 0811.3982 , Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID   118577511.
  8. 1 2 Fuhrmann, Klaus (2011). "Nearby stars of the Galactic disc and halo - V". Monthly Notices of the Royal Astronomical Society. 414 (4): 2893–2922. Bibcode:2011MNRAS.414.2893F. doi: 10.1111/j.1365-2966.2011.18476.x .
  9. ↑ 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.
  10. 1 2 "SolStation: HR 483 / HD 10307 AB".
  11. ↑ P. M. Bagnall (2012). The Star Atlas Companion: What you need to know about the Constellations. Bibcode:2012sacw.book.....B.
  12. ↑ Halbwachs, J. -L; Mayor, M.; Udry, S.; Fekel, F. C.; Hartkopf, W. I.; Levato, H.; Morrell, N. I.; Torres, G.; Udry, S. (2018). "Multiplicity among solar-type stars. IV. The CORAVEL radial velocities and the spectroscopic orbits of nearby K dwarfs". Astronomy and Astrophysics. 619: A81. arXiv: 1808.04605 . Bibcode:2018A&A...619A..81H. doi:10.1051/0004-6361/201833377. S2CID   119437322.
  13. ↑ Lubin, Dan; Tytler, David; Kirkman, David (March 2012), "Frequency of Maunder Minimum Events in Solar-type Stars Inferred from Activity and Metallicity Observations", The Astrophysical Journal Letters, 747 (2): L32, Bibcode:2012ApJ...747L..32L, doi: 10.1088/2041-8205/747/2/L32 .
  14. ↑ Rodriguez, David R.; Duchêne, Gaspard; Tom, Henry; Kennedy, Grant M.; Matthews, Brenda; Greaves, Jane; Butner, Harold (2015). "Stellar multiplicity and debris discs: An unbiased sample". Monthly Notices of the Royal Astronomical Society. 449 (3): 3160. arXiv: 1503.01320 . Bibcode:2015MNRAS.449.3160R. doi: 10.1093/mnras/stv483 .
  15. ↑ (in Russian) http://www.cplire.ru/rus/ra&sr/VAK-2004.html Archived 2019-05-30 at the Wayback Machine
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