HD 23523

HD 23523
Location of HD 23523 on the map (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Camelopardalis
Right ascension 03h 49m 36.58592s[1]
Declination +63° 17′ 49.0518″[1]
Apparent magnitude (V) 5.82[2] (6.31 + 7.11)[3]
Characteristics
Spectral type A5 Vn[4]
B−V color index +0.18[5]
Astrometry
Radial velocity (Rv)−9.6±3.4[6] km/s
Proper motion (μ) RA: −11.630 mas/yr[1]
Dec.: −61.457 mas/yr[1]
Parallax (π)13.9498 ± 0.3245 mas[1]
Distance234 ± 5 ly
(72 ± 2 pc)
Absolute magnitude (MV)+1.55[7] (combined)
Orbit[8]
PrimaryHD 23523A[3]
CompanionHD 23523B[3]
Period (P)10.180±0.509 yr
Semi-major axis (a)0.1020±0.0031″
Eccentricity (e)0.441
Details
A
Mass1.75 or 1.81[9] M☉
B
Mass1.64 or 1.51[9] M☉
Other designations
Moaï 1, AG+63°280, BD+62°612, GC 4560, HD 23523, HIP 17891, HR 1158, SAO 12917, WDS J03496+6318AB[10]
Database references
SIMBADdata

HD 23523 (HR 1158) is a binary star[11] located in the northern circumpolar constellation Camelopardalis. It has a combined apparent magnitude of 5.82,[2] making it faintly visible to the naked eye under ideal conditions. When resolved, the primary has an apparent magnitude of 6.31 while the secondary has a magntiude of 7.11.[3] The system is located relatively close at a distance of about 234 light-years based on Gaia DR3 parallax measurements[1] and it currently drifting closer with a somewhat heliocentric radial velocity of −9.6 km/s.[6] At its current distance, HD 23523's combined brightness is diminished by 0.16 magnitudes due to interstellar extinction[12] and it has a combined absolute magnitude of +1.55.[7]

The system was first discovered to be a double star in 1996 by Marcel Carbillet and colleagues after speckle interferometry observations.[13] The stars are only about a tenth of an arcsecond apart,[3] making observing their individual properties difficult. The discovery paper suggested that the two components might be equal based on the dynamical mass.[13] Overall, HD 23523 has a stellar classification of A5 Vn,[4] indicating that it is an A-type main-sequence star with broad or nebulous absorption lines due to rapid rotation. The primary has a mass either 1.75 or 1.81 times the mass of the Sun while the companion has a mass 1.64 or 1.51 times that of the Sun,[9] depending on the approach.

  1. ^ a b c d e Cite error: The named reference GaiaDR3 was invoked but never defined (see the help page).
  2. ^ a b Cite error: The named reference Tycho2000 was invoked but never defined (see the help page).
  3. ^ a b c d e Cite error: The named reference Mason2001 was invoked but never defined (see the help page).
  4. ^ a b Cite error: The named reference Cowley1969 was invoked but never defined (see the help page).
  5. ^ Cite error: The named reference Ljuggren1965 was invoked but never defined (see the help page).
  6. ^ a b Cite error: The named reference Gontcharov2006 was invoked but never defined (see the help page).
  7. ^ a b Cite error: The named reference Anderson2012 was invoked but never defined (see the help page).
  8. ^ Cite error: The named reference Malkov2012 was invoked but never defined (see the help page).
  9. ^ a b c Cite error: The named reference Cvetkovic2010 was invoked but never defined (see the help page).
  10. ^ Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  11. ^ Cite error: The named reference Eggleton2008 was invoked but never defined (see the help page).
  12. ^ Cite error: The named reference Gontcharov2017 was invoked but never defined (see the help page).
  13. ^ a b Cite error: The named reference Carbillet1996 was invoked but never defined (see the help page).