01h48m 41.56269s[1]
+32° 41′ 24.7521″[1]
5.81[2]
Characteristics
F8 V[3]
U−B color index
−0.03[2]
B−V color index
+0.54[2]
Radial velocity (Rv)
−24.4±0.3[4] km/s
Proper motion (μ)
RA: −167.798 mas/yr[1]
Dec.: +296.869 mas/yr[1]
Parallax (π)
90.4 ± 0.1 ly
(27.71 ± 0.04 pc)
Absolute magnitude (MV)
+3.56[5]
Details
Surface gravity (log g)
Metallicity [Fe/H]
Rotational velocity (v sin i)
5±3[10] km/s
Database references
HD 11007 (LTT 10624; HR 523) is a probable astrometric binary[13] located in the northern constellation Triangulum. The primary is faintly visible to the naked eye as a whitish-yellow-hued star with an apparent magnitude of 5.81.[2] The system is located relatively close at a distance of 90.4 light-years based on Gaia DR3 parallax measurements[1] and it is drifting closer with a heliocentric radial velocityof−24.4 km/s.[4] At its current distance, HD 11007's brightness is diminished by an interstellar extinction of 0.09 magnitudes[14] and it has an absolute magnitude of +3.56.[5] It is moving relatively fast across the celestial sphere,[15] having a high proper motion of 341 mas/yr.[1]
The primary has a stellar classification of F8 V,[3] indicating that it is an ordinary F-type main-sequence star that is generating energy via hydrogen fusion at its core. However, it is slightly evolved, being 1.62 magnitudes above the zero age main sequence.[16] It has 111% the mass of the Sun[6] and a slightly enlarged radius 1.67 times that of the Sun.[7] It is slightly over luminous for its class, radiating 3.23 times the luminosity of the Sun[1] from its photosphere at an effective temperatureof6,060 K.[7] HD 11007 A is metal deficient with an iron abundance that is 63.1% solar[9] and it spins modestly with a somewhat constrained projected rotational velocity of approximately 5 km/s.[10] The system is estimated to be 6.6 billion years old; it was suspected to be part of the thick disk population[11] but is now considered to be one of the older members of the thin disk population.[17]
Other
Numbered
Other