HD 10307

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HD 10307 A/B
Observation data Epoch J2000.0 Equinox J2000.0
Constellation	Andromeda
Right ascension	01^h 41^m 47.143^s^[1]
Declination	+42° 36′ 48.12″^[1]
Apparent magnitude (V)	+4.95/+12.5
Characteristics
Spectral type	G1.5 V + M V
U−B color index	0.11
B−V color index	0.62
Variable type	None
Astrometry

Radial velocity (R_v)	+3.1 km/s
Proper motion (μ)	RA: 791.47 ± 0.48^[1] mas/yr Dec.: -180.80 ± 0.36^[1] mas/yr
Parallax (π)	78.50 ± 0.54^[1] mas
Distance	41.5 ± 0.3 ly (12.74 ± 0.09 pc)
Absolute magnitude (M_V)	4.30/11.9

Details
HD 10307 A
Mass	0.97^[2] M_☉
Radius	1.20 R_☉
Luminosity	1.44 L_☉
Surface gravity (log g)	4.35 cgs
Temperature	5,881 ± 4.0^[3] K
Metallicity	96% Sun
Age	7.0 × 10⁹^[4] years
HD 10307 B
Mass	0.29 M_☉
Luminosity	0.0013 L_☉
Orbit
Companion	HR 483 B
Period (P)	19.5 yr
Semi-major axis (a)	0.58"
Eccentricity (e)	0.43
Inclination (i)	103°
Other designations
BD+41 328, GJ 67, HD 10307, HIP 7918, HR 483, LHS 1284, NStars 0141+4236, SAO 37434, YPC 350
Database references
SIMBAD	data
ARICNS	data

HD 10307 (HR 483 A) is a star similar to the Sun in mass, temperature and metal content, situated about 41 light-years from Earth in the constellation Andromeda. Its companion, HR 483 B, is a little-studied red dwarf.

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.

System

HR 483 is a binary located 41.2 ly away, in Andromeda. The two stars orbit one another elliptically (e=0.43), approaching as close as 4.2 AU and receding to 10.5 AU, with a period of just under twenty years. Due to the high margins of error on the mass estimates for the two stars, these orbital parameters are approximate.

HD 10307, the larger component, is a main sequence, yellow, sun-like star, only slightly brighter, hotter, and larger than the Sun. It has a low level of activity and is a candidate Maunder minimum analog.^[2] HR 483 B, the smaller component, appears to be a red dwarf, with as little as thirty percent the mass of the sun.

Possibility of planets and life

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.

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.^[5]

References

↑ 1.0 1.1 1.2 1.3 1.4 van Leeuwen, F. (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. Vizier catalog entry
↑ 2.0 2.1 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.
↑ Kovtyukh et al. (2003). "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios". Astronomy and Astrophysics 411 (3): 559–564. arXiv:astro-ph/0308429. Bibcode:2003A&A...411..559K. doi:10.1051/0004-6361:20031378.
↑ 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.
↑ (Russian) http://www.cplire.ru/rus/ra&sr/VAK-2004.html

External links

Wikimedia Commons has media related to Canes Venatici.

← Star systems within 40–45 light-years →

Star systems (including brown dwarf systems) within 40–45 light-years from Earth.

Giant star

G III	Capella (42.2 ± 0.5 ly; 4 stars)

F
(Yellow-white)

IV	Beta Trianguli Australis (40.2 ± 0.3 ly; 2 stars) Theta Ursae Majoris «Alhaud» (44.0 ± 0.4 ly; 3 stars)

V	36 Ursae Majoris (41.9 ± 0.4 ly; 2 stars) Upsilon Andromedae (43.9 ± 0.4 ly; 2 stars, 4 planets: b c d e) 10 Tauri (44.8 ± 0.5 ly; 2 stars) Iota Piscium (45.0 ± 0.5 ly; 1 star)

G
(Yellow)

IV	Beta Aquilae «Alshain» (44.7 ± 0.5 ly; 2 stars)

V	Rho¹ (55) Cancri (40.9 ± 0.4 ly; 2 stars, 5 planets: e b c f d) HR 483 (41.2 ± 0.4 ly; 2 stars) Lambda Aurigae «Al Hurr» (41.2 ± 0.5 ly; 2 stars) HR 683 (41.4 ± 0.4 ly; 1 star) i (44) Boötis (41.6 ± 0.3 ly; 3 stars) HD 147513 (42.0 ± 0.5 ly; 2 stars, 1 planet: b) HR 6998 (42.4 ± 0.5 ly; 1 star) 58 Eridani (43.4 ± 0.5 ly; 1 star) HR 8501 (44.4 ± 0.4 ly; 2 stars)

K
(Orange)

IV	HR 4587 (42.1 ± 0.4 ly; 1 star) Gamma Cephei «Errai» (45.0 ± 0.3 ly; 2 stars, 1 planet: b)

V	Gliese 435 (40.8 ± 0.5 ly; 1 star) HD 69830 (41.0 ± 0.4 ly; 1 star, 3 planets: b c d) Gliese 142 (41.2 ± 1.2 ly; 1 star) Gliese 349 (41.4 ± 0.6 ly; 1 star) HD 158633 (41.7 ± 0.3 ly; 1 star) HD 40307 (41.8 ± 0.3 ly; 1 star, 6 planets: b c d e f g) Gliese 428 (42.0 ± 1.0 ly; 2 stars) HD 166348 (42.3 ± 0.7 ly; 1 star) Gliese 204 (42.3 ± 0.5 ly; 1 star) Gliese 167 (42.7 ± 0.3 ly; 1 star) HD 190007 (42.8 ± 0.6 ly; 1 star) SZ Crateris (42.9 ± 1.0 ly; 2 stars) HD 170657 (43.1 ± 0.5 ly; 1 star) Gliese 146 (43.6 ± 0.5 ly; 1 star) GJ 1267 (43.6 ± 0.8 ly; 1 star) Gliese 556 (43.8 ± 0.4 ly; 1 star) Gliese 69 (43.8 ± 0.7 ly; 1 star) HD 29697 (44.0 ± 0.8 ly; 1 star) Gliese 868 (44.2 ± 0.7 ly; 1 star) Gliese 528 (44.4 ± 0.7 ly; 2 stars) HD 154577 (44.6 ± 0.6 ly; 1 star) HD 166 (44.7 ± 0.5 ly; 2 stars) Gliese 615 (44.8 ± 0.5 ly; 1 star)

M V (Red dwarf)	Gliese 179 (40.1+2.1 −1.9 ly; 1 star, 1 planet: b) Gliese 806 (40.2 ± 0.9 ly; 1 star) GJ 4360 (40.8 ± 0.7 ly; 2 stars) HD 175224 (41.2 ± 1.6 ly; 2 stars) GJ 3707 (41.9 ± 1.3 ly; 1 star) Gliese 521 (42.4 ± 0.9 ly; 1 star) Gliese 215 (44.7 ± 0.7 ly; 1 star)

White
dwarf

DA	G 29-38 (44.4+2.6 −2.3 ly; 1 star)

DC	GRW +70 8247 (42.4+1.3 −1.2 ly; 1 star)

Brown
dwarf

T	WISE J0457-0207 (40.8* ± 10.1 ly; 1 brown dwarf)* WISE 1051-2138 (~40.8 ly; 1 brown dwarf) ULAS J0034-00 (41.0+2.1 −1.9 ly; 1 brown dwarf) WISE 1542+2230 (~41.1 ly; 1 brown dwarf) WISE 0857+5604 (~42.1 ly; 1 brown dwarf) WISE 2019-1148 (~42.4 ly; 1 brown dwarf) WISE 2134-7137 (~42.7 ly; 1 brown dwarf) WISE 2359-7335 (~42.7 ly; 1 brown dwarf) WISE 1311+0122 (~44.4 ly; 1 brown dwarf) WISE 1952+7240 (~44.4 ly; 1 brown dwarf) WISE 0513+0608 (~44.7 ly; 1 brown dwarf) WISE 2255-3118 (~44.7 ly; 1 brown dwarf) WISE 2226+0440 (~45.0 ly; 1 brown dwarf)

Y	WISE 1541-2250 (44.1+31.8 −13.0 ly; 1 brown dwarf)

In left column are stellar classes of primary members of star systems. Bold are systems containing at least one component with absolute magnitude of +8.5 or brighter. Italic are systems without known trigonometric parallax.

v t e Stars of Andromeda

Bayer	α (Alpheratz) β (Mirach) γ (Almach) δ ε ζ η θ ι κ λ μ ν ξ (Adhil) ο π ρ σ τ υ φ χ ψ ω

Flamsteed	2 3 4 5 6 7 8 9 10 11 12 13 14 15 18 22 23 26 28 32 36 39 41 44 45 47 49 51 55 56 58 59 60 62 63 64 65 66 6 Per

Variable	R S T U V W X Y Z RR RS RT RU RV RW RX RY SS ST SU SW TU TW VX WZ XX XZ AB AC AD AE AF AR BM BX CC CG CN DS DX EG ET EU FF GO GP GR GY HN KK KX KZ LL LN LP LQ OP OS OU PX PY QR QX V385 V455 V529

HR	1 8 17 36 40 44 52 53 56 71 75 78 79 104 110 122 134 152 156 157 178 205 249 272 275 282 289 355 372 376 379 396 409 415 452 483 495 504 518 521 551 552 556 619 647 653 671 673 679 687 746 748 756 768 769 8744 8801 8837 8857 8875 8884 8925 8927 8941 8950 8955 8962 8973 8977 8986 9011 9053 9057 9074 9086 9105 9107

HD	800 8673 11884 13931 14633 15082 217731 218365 218393 218915 222155

Other	ADS 48 Groombridge 34 HAT-P-6 HAT-P-16 HAT-P-19 HAT-P-28 HAT-P-32 M31V J004437.99+412923.6 PSR B2303+46 PSR J0218+4232 Ross 248 WASP-1 WISE 0146+4234

List

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