  | |
| Observation data EpochJ2000.0 EquinoxJ2000.0 | |
|---|---|
| Constellation | Cassiopeia[1] |
| Right ascension | 23h 57m 08.47206s[2] |
| Declination | +55° 42′ 20.5393″[2] |
| Apparent magnitude (V) | 5.57 - 5.68[3] |
| Characteristics | |
| Spectral type | F6V[4] |
| Variable type | Algol[3] |
| Astrometry | |
| Proper motion (μ) | RA: −20.899±0.042[2]mas/yr Dec.: −12.336±0.041[2]mas/yr |
| Parallax (π) | 15.7172±0.0463 mas[2] |
| Distance | 207.5 ± 0.6 ly (63.6 ± 0.2 pc) |
| Absolute magnitude (MV) | +1.32[1] |
| Orbit[4] | |
| Period (P) | 12.1561594±0.0000006 d |
| Semi-major axis (a) | 32.903±0.003 R☉ |
| Eccentricity (e) | 0.3115±0.0001 |
| Inclination (i) | 82.925±0.025° |
| Details | |
| Primary | |
| Mass | 1.626±0.001[4] M☉ |
| Radius | 2.570±0.021[4] R☉ |
| Luminosity | 9.67±1.08[4] L☉ |
| Temperature | 6,350±150[4] K |
| Age | 1.9[5] Gyr |
| Secondary | |
| Mass | 1.607±0.001[4] M☉ |
| Radius | 2.445±0.022[4] R☉ |
| Luminosity | 9.15±0.97[4] L☉ |
| Temperature | 6,420±150[4] K |
| Age | 1.9[5] Gyr |
| Other designations | |
| V1022 Cas,BD+54 3076,HIP 118077,HR 9059,Boss 6148,SAO 35917[6] | |
| Database references | |
| SIMBAD | data |
HD 224355, also known asV1022 Cassiopeiae,HR 9059 and (in early publications)Boss 6148, is aneclipsing binary star in the constellationCassiopeia. It ranges inapparent magnitude from 5.57 to 5.68, which means it is faintly visible to thenaked eye for an observer located well away fromcity lights.[3] It is one of the few binaries known to be anastrometric,spectroscopic and eclipsing binary, a combination that allows the parameters of the stellar system to be calculated with high accuracy.[7] HD 224355 lies16′ west of the 5th-magnitudeσ Cassiopeiae.
HD 224355 was discovered to be a spectroscopic binary byHarry Hemley Plaskett of theDAO, in 1919.[9] Many additional spectra were obtained at the DAO in 1922, andorbital elements of the binary were first published in 1923. The orbit was found to have a significant eccentricity of 0.278.[10] Because the physical separation of spectroscopic binaries is often relatively small, they are good candidates to be eclipsing binaries. For that reason, in 1924 Joel Stebbins included HD 224355 in an early photo-electric photometry study, and observed a "suspect eclipse".[11] That led to the star being listed in theNew Catalogue of Suspected Variable Stars as NSV 14773.[12]Hipparcos data confirmed that HD 224355 is anAlgol-type eclipsing binary.[13] In 2008 it was given thevariable star designation V1022 Cassiopeiae.[14]
From 2014 through 2017, HD 224355 was observed with theCHARAoptical interferometer. Those observations allowed the orbit to be directly traced from the changes of the stars' relative positions on the sky. That orbit, when combined withradial velocity information, provided a distance measurement to the star. The value obtained,63.98±0.26 pc, agrees well with the value of63.6±0.2 pc measured by theGaia spacecraft using the completely independent method ofstellar parallax.[5]
Both components of the HD 224355 system are slightly more massive than the Sun, F5 or F6 stars 1.9 billion years old and right at the end of theirmain sequence lives. Each is about 2.5 times theradius of the Sun and 9 or 10 timesas luminous, and they haveeffective temperatures around6,400 K.[4]
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