HD 224355

HD 224355
	Location of HD 224355 (circled)
Observation data; Epoch J2000.0 Equinox J2000.0
Constellation	Cassiopeia
Right ascension	23h 57m 08.47206s
Declination	+55° 42′ 20.5393″
Apparent magnitude (V)	5.57 - 5.68
Characteristics
Spectral type	F6V
Variable type	Algol
Astrometry
Proper motion (μ)	RA: −20.899±0.042 mas/yr ; Dec.: −12.336±0.041 mas/yr
Parallax (π)	15.7172 ± 0.0463 mas
Distance	207.5 ± 0.6 ly ; (63.6 ± 0.2 pc)
Orbit
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 M☉
Radius	2.570±0.021 R☉
Luminosity	9.67±1.08 L☉
Temperature	6,350±150 K
Age	1.9 Gyr
Secondary
Mass	1.607±0.001 M☉
Radius	2.445±0.022 R☉
Luminosity	9.15±0.97 L☉
Temperature	6,420±150 K
Age	1.9 Gyr
Other designations
	V1022 Cas, BD+54 3076, HIP 118077, HR 9059, Boss 6148, SAO 35917
Database references
SIMBAD	data

HD 224355, also known as V1022 Cassiopeiae, HR 9059 and (in early publications) Boss 6148, is an eclipsing binary star in the constellation Cassiopeia. It ranges in apparent magnitude from 5.57 to 5.68, which means it is faintly visible to the naked eye for an observer located well away from city lights.^[2] It is one of the few binaries known to be an astrometric, spectroscopic and eclipsing binary, a combination that allows the parameters of the stellar system to be calculated with high accuracy.^[6] HD 224355 lies 16′ west of the 5th-magnitude σ Cassiopeiae.

A light curve for HD 224355, plotted from *TESS* data^[7]

HD 224355 was discovered to be a spectroscopic binary by Harry Hemley Plaskett of the DAO, in 1919.^[8] Many additional spectra were obtained at the DAO in 1922, and orbital elements of the binary were first published in 1923. The orbit was found to have a significant eccentricity of 0.278.^[9] 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".^[10] That led to the star being listed in the New Catalogue of Suspected Variable Stars as NSV 14773.^[11] Hipparcos data confirmed that HD 224355 is an Algol-type eclipsing binary.^[12] In 2008 it was given the variable star designation V1022 Cassiopeiae.^[13]

From 2014 through 2017, HD 224355 was observed with the CHARA optical 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 with radial velocity information, provided a distance measurement to the star. The value obtained, 63.98±0.26 pc, agrees well with the value of 63.6±0.2 pc measured by the Gaia spacecraft using the completely independent method of stellar parallax.^[4]

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 their main sequence lives. Each is about 2.5 times the radius of the Sun and 9 or 10 times as luminous, and they have effective temperatures around 6,400 K.^[3]

References

^ ^a ^b ^c ^d ^e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
^ ^a ^b ^c Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j ^k Fekel, Francis C.; Henry, Gregory W.; Sowell, James R.; Partington, Ethan R.; Wedemeyer, Joanna M.; Nakum, ArjunSinh (November 2022). "An Analysis of the Eclipsing Binaries HD 71636, V1022 Cassiopeiae, and OT Andromedae". The Astronomical Journal. 164 (5): 224. Bibcode:2022AJ....164..224F. doi:10.3847/1538-3881/ac84de. S2CID 253203467.
^ ^a ^b ^c Lester, Kathryn V.; Gies, Douglas R.; Schaefer, Gail H.; Farrington, Christopher D.; Monnier, John D.; ten Brummelaar, Theo; Sturmann, Judit; Vargas, Norman (April 2019). "Visual Orbits of Spectroscopic Binaries with the CHARA Array. I. HD 224355". The Astronomical Journal. 157 (4): 140. arXiv:1902.05557. Bibcode:2019AJ....157..140L. doi:10.3847/1538-3881/ab064d. S2CID 119283523.
^ "V1022 Cas -- Spectroscopic Binary". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2023-01-09.
^ Southworth, J. (April 2021). "Rediscussion of eclipsing binaries. Paper 3: The interferometric, spectroscopic, and eclipsing binary V1022 Cassiopeiae". The Observatory. 141: 52–63. arXiv:2012.05978. Bibcode:2021Obs...141...52S.
^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 11 January 2023.
^ Plaskett, J. S.; Harper, W. E.; Young, R. K.; Plaskett, H. H. (January 1920). "One hundred spectroscopic binaries". Publications of the Dominion Astrophysical Observatory Victoria. 1: 163–185. Bibcode:1920PDAO....1..163P.
^ Harper, W. (April 1923). "The Orbits of the Spectroscopic Components of Boss 6148". Publications of the Dominion Astrophysical Observatory Victoria. 2: 263–267. Bibcode:1923PDAO....2..263H.
^ Stebbins, Joel (January 1928). "Photo-Electric Photometry of Stars". Publications of the Washburn Observatory. 15: ii-213. Bibcode:1928PWasO..15D...2S.
^ "New Catalogue of Suspected Variable Stars: The Improved Version". Sternberg Astronomical Institute. Moscow University.
^ Otero, S. (May 2006). "Observations of Variables" (PDF). Information Bulletin on Variable Stars. 5699: 1. Bibcode:2006IBVS.5699....1. Retrieved 12 January 2023.
^ Kazarovets, E. V.; Samus, N. N.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (November 2008). "The 79th Name-List of Variable Stars". Information Bulletin on Variable Stars. 5863: 1. Bibcode:2008IBVS.5863....1K.