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V389 Cygni

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V389 Cygni, also known as HD 201433 and HR 8094, is a star about 390 light years from the Earth, in the constellation Cygnus. It is a 5th-magnitude star, making it faintly visible to the naked eye of an observer far from city lights. V389 Cygni is a multiple star.[4] One component of that system is a slowly pulsating B-type star (SPB) causing the system's brightness to vary from magnitude 5.55 to 5.71 over a period of 1.4 days.[6]

V389 Cygni
Location of V389 Cygni (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cygnus
A
Right ascension 21h 08m 38.88974s[1]
Declination +30° 12′ 20.2879″[1]
Apparent magnitude (V) 5.712[2]
B
Right ascension 21h 08m 38.67181s[3]
Declination +30° 12′ 22.2133″[3]
Apparent magnitude (V) 8.060[2]
Characteristics
Spectral type B9V[4]
(B9VspSi + kA2.5hA7VmA9n)[5]
Variable type Slowly pulsating B[6]
Astrometry
A
Proper motion (μ) RA: +24.645[1] mas/yr
Dec.: −20.647[1] mas/yr
Parallax (π)8.1988 ± 0.1038 mas[1]
Distance398 ± 5 ly
(122 ± 2 pc)
B
Proper motion (μ) RA: +24.004[3] mas/yr
Dec.: −25.161[3] mas/yr
Parallax (π)8.4500 ± 0.0263 mas[3]
Distance386 ± 1 ly
(118.3 ± 0.4 pc)
Orbit[7]
PrimaryAa1
CompanionAa2
Period (P)3.313 d
Eccentricity (e)0
Semi-amplitude (K1)
(primary)		21.77 km/s
Orbit[7]
PrimaryAa
CompanionAb
Period (P)154.072 d
Eccentricity (e)0.311
Semi-amplitude (K1)
(primary)		9.49 km/s
Details
Aa1
Mass3.17[8] M☉
Radius2.5[9] R☉
Luminosity113[9] L☉
Surface gravity (log g)4.14[9] cgs
Temperature11,885[9] K
Rotation1.13 d[10]
Rotational velocity (v sin i)17.9[11] km/s
Aa2
Mass0.40 M☉
Ab
Mass0.65 M☉
B
Mass1.54[8] M☉
Radius1.5[9] R☉
Luminosity6.2[9] L☉
Surface gravity (log g)4.33[9] cgs
Temperature7,482[9] K
Rotational velocity (v sin i)77[11] km/s
Other designations
HD 201433, BD+29 4324, HIP 104371, HR 8094, SAO 70968, ADS 14682 AB[12] Boss 5442,[13] WDS 21086+3012AB[14]
Database references
SIMBADdata
A
B

V389 Cygni is catalogued as a multiple star with four visible components. The faint companions TYC 2701-897-1 and UCAC4 602-123109 are unrelated background objects,[15] at 59″ and 73″ respectively.[16] A 5th-magnitude and 8th-magnitude star separated by 3.3″ form a common proper motion pair, generall referred to as components A and B). The brighter star, component A, is a spectroscopic binary and the system also harbours an unseen third star, making it a triple and the system as a whole then includes four stars.[8] Both the visible stars are chemically peculiar, A being an Ap star and B an Am star.[17] The blended spectral class of the pair is B9V, with the brighter star having a class of B9VspSi (or B9 Si Mg)[17] and the fainter kA2.5hA7VmA9n.

Component A of V389 Cygni was discovered to be a spectroscopic binary from spectra obtained in 1918. In 1921, Reynold K. Young of the Dominion Astrophysical Observatory derived its orbit from 49 additional spectra obtained in 1920-1921. He found it to have a circular orbit, with a period of 3.3137 days. He noted that the star showed evidence of variability.[13]

A light curve for V389 Cygni, plotted from TESS data.[18] The 1.4289 day period[6] is marked in red.

In 1922 Kurt Bottlinger and Paul Guthnick detected variability in V389 Cygni.[19] Between 1936 and 1942, Guthnick made extensive photoelectric observations of V389 Cygni. He found that sometimes the brightness appeared to change irregularly, and at other times two periods, 1.12912 and 1.19328 days, could be seen. Neither period was related to the orbital period of the spectroscopic binary. Guthnick postulated that the system consisted of two Cepheid variables orbiting each other,[20][21] but it is now believed that only one of the stars in the close binary pair is variable, and it is an SPB star.[4]

In 1978, Frank Gieseking and Wilhelm Seggewiss refined Young's orbit determination for the spectroscopic binary (new period 3.313168±0.000008 days), and found that V389 Cygni is a triple star. The third, unseen component, orbits the close binary pair with a period of 154.09±0.02 days. They were unable to derive a nonzero eccentricity for either orbit.[19] In 1989, David Barlow re-analyzed earlier data and found that while the orbit of the inner binary appeared to be circular, the data were best fit if the orbit of the third star had an eccentricity of 0.311±0.057.[7]

In 2017, Thomas Kallinger et al. published an extensive spectroscopic and astroseismic study of V389 Cygni. They found 29 pulsation frequencies in the BRITE satellite data for the star. They were able to derive an eccentricity value for the inner binary pair's orbit of 0.015±0.003. Their astroseismic results indicate that the outer layer of the SPB star is in the process of becoming tidally locked to its close companion, but the inner portion of the star still rotates at a significantly different speed.[4]

References

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  1. ^ 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.
  2. ^ a b Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN 0004-6361.
  3. ^ 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.
  4. ^ a b c d Kallinger, T.; Weiss, W. W.; Beck, P. G.; Pigulski, A.; Kuschnig, R.; Tkachenko, A.; Pakhomov, Y.; Ryabchikova, T.; Lüftinger, T.; Palle, P. L.; Semenko, E.; Handler, G.; Koudelka, O.; Matthews, J. M.; Moffat, A. F. J.; Pablo, H.; Popowicz, A.; Rucinski, S.; Wade, G. A.; Zwintz, K. (July 2017). "Triple system HD 201433 with a SPB star component seen by BRITE - Constellation: Pulsation, differential rotation, and angular momentum transfer" (PDF). Astronomy and Astrophysics. 603: A13. arXiv:1704.01151. Bibcode:2017A&A...603A..13K. doi:10.1051/0004-6361/201730625. S2CID 119411639. Retrieved 21 January 2023.
  5. ^ Abt, H. A.; Cardona, O. (1984). "The nature of the visual companions of AP and AM stars". The Astrophysical Journal. 276: 266. Bibcode:1984ApJ...276..266A. doi:10.1086/161610.
  6. ^ a b c "V0389 Cyg". International Variable Star Index. AAVSO. Retrieved 21 January 2023.
  7. ^ a b c Barlow, D. J. (December 1989). "On the circularity of the orbits of the triple system V389 Cygni". The Observatory. 109: 225–229. Bibcode:1989Obs...109..225B. Retrieved 21 January 2023.
  8. ^ a b c Tokovinin, Andrei (2018-03-01). "The Updated Multiple Star Catalog". The Astrophysical Journal Supplement Series. 235 (1): 6. arXiv:1712.04750. Bibcode:2018ApJS..235....6T. doi:10.3847/1538-4365/aaa1a5. ISSN 0067-0049. S2CID 119047709.
  9. ^ a b c d e f g h Stassun, Keivan G.; et al. (9 September 2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694. Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467. eISSN 1538-3881. hdl:1721.1/124721. S2CID 166227927.
  10. ^ Oelkers, Ryan J.; Rodriguez, Joseph E.; Stassun, Keivan G.; Pepper, Joshua; Somers, Garrett; Kafka, Stella; Stevens, Daniel J.; Beatty, Thomas G.; Siverd, Robert J.; Lund, Michael B.; Kuhn, Rudolf B.; James, David; Gaudi, B. Scott (2018). "Variability Properties of Four Million Sources in the TESS Input Catalog Observed with the Kilodegree Extremely Little Telescope Survey". The Astronomical Journal. 155 (1): 39. arXiv:1711.03608. Bibcode:2018AJ....155...39O. doi:10.3847/1538-3881/aa9bf4. S2CID 119515775.
  11. ^ a b Glebocki, R.; Gnacinski, P. (2005). "VizieR Online Data Catalog: Catalog of Stellar Rotational Velocities (Glebocki+ 2005)". VizieR On-line Data Catalog: III/244. Originally Published in: 2005csss...13..571G; 2005yCat.3244....0G. 3244. Bibcode:2005yCat.3244....0G.
  12. ^ "HD 201433 -- Double or Multiple Star". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2023-01-21.
  13. ^ a b Young, R. K. (1921). "Orbit of the spectroscopic binary Boss 5442". Publications of the Dominion Astrophysical Observatory Victoria. 1: 319–323. Bibcode:1921PDAO....1..319Y. Retrieved 21 January 2023.
  14. ^ Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (December 2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi:10.1086/323920. S2CID 119533755.
  15. ^ Hoffleit, Dorrit; Jaschek, Carlos (1991). "The Bright star catalogue". New Haven, Conn.: Yale University Observatory, 5th Rev.ed. Bibcode:1991bsc..book.....H.
  16. ^ Mason, Brian D.; et al. (December 2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.
  17. ^ a b Renson, P.; Manfroid, J. (May 2009). "Catalogue of Ap, HgMn and Am stars". Astronomy and Astrophysics. 498 (3): 961–966. Bibcode:2009A&A...498..961R. doi:10.1051/0004-6361/200810788.
  18. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 16 January 2023.
  19. ^ a b Gieseking, F.; Seggewiss, W. (August 1978). "Spectroscopic investigation of the peculiar binary V389 Cyg". Astronomy and Astrophysics. 68: 437–441. Bibcode:1978A&A....68..437G. Retrieved 21 January 2023.
  20. ^ Gieseking, F. (April 1979). "Photoelectric observations of the peculiar variable V389 Cygni". Astronomy and Astrophysics Supplement Series. 36: 37–43. Bibcode:1979A&AS...36...37G. Retrieved 21 January 2023.
  21. ^ Hoffleit, Dorrit (May 1977). "Wanted: Photoelectric and Spectroscopic Observations of the Unusual System, V389 Cygni" (PDF). Information Bulletin on Variable Stars. 1283: 1. Bibcode:1977IBVS.1283....1H. Retrieved 21 January 2023.
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