U Lacertae

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U Lacertae
Lacerta constellation map.svg
Red circle.svg
Location of U Lacertae (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Lacerta
Right ascension 22h 47m 43.42677s [1]
Declination 55° 09′ 30.3036″ [1]
Apparent magnitude  (V)9.40 [2]
Characteristics
Spectral type M4epIab + B [3]
U−B color index +1.46 [2]
B−V color index +2.34 [2]
Variable type SRc [3]
Astrometry
Radial velocity (Rv)−68 [4]  km/s
Proper motion (μ)RA: −3.207 [5]   mas/yr
Dec.: −3.150 [5]   mas/yr
Parallax (π)0.3519 ± 0.0708  mas [5]
Distance 2,750 [6]   pc
Absolute magnitude  (MV)−5.6 [7]
Details
Mass 22 [7]   M☉
Radius 1,013 [8]   R☉
Luminosity 152,000 [8]   L☉
Temperature 3,535 [8]   K
Other designations
U  Lac, HIP  112545, PPM  411, GSC  03988-01641, IRC+50446, TYC  3988-1641-1, BD+54° 2863, HD  215924, 2MASS  J22474341+5509303, AAVSO  2243+54
Database references
SIMBAD data

U Lacertae is a spectroscopic binary star in the constellation Lacerta.

Despite being in the constellation of Lacerta, U Lacertae is considered to be a member of the Cepheus OB1 association. [9] It has been listed as a member of the open cluster ASCC 123. [10]

U Lacertae is a binary star consisting of a red supergiant and a small hot companion, similar to VV Cephei. The companion has been identified from a high excitation component in the spectrum and from radial velocity variations, but the orbit is unknown. [11]

A visual band light curve for U Lacertae, plotted from AAVSO data ULacLightCurve.png
A visual band light curve for U Lacertae, plotted from AAVSO data

In 1894, T. H. E. C. Espin announced that the star, then called BD +54° 2863, might be a variable star. [13] T. W. Blackhouse confirmed its variability in 1897. [14] It was listed with its variable star designation, U Lacertae, in Annie Jump Cannon's 1907 work Second Catalog of Variable Stars. [15] U Lacertae is classified as a semiregular variable. [3] The periodicity is uncertain but a main period of 150 days and a long secondary period of 550 – 690 days have been suggested. [16] A study of Hipparcos satellite photometry found an amplitude of 0.77 magnitudes and found no periodicity. [17] The General Catalogue of Variable Stars lists an amplitude of 2.7 magnitudes. [3]

Water masers have been detected around U Lacertae, common in the extended atmospheres of very luminous cool stars. [18]

See also

Related Research Articles

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<span class="mw-page-title-main">Nu Cephei</span> Star in the constellation Cepheus

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<span class="mw-page-title-main">W Cephei</span> Variable star in the constellation Cepheus

W Cephei is a spectroscopic binary and variable star located in the constellation Cepheus. It is thought to be a member of the Cep OB1 stellar association at about 8,000 light years. The supergiant primary star is one of the largest known stars and as well as one of the most luminous red supergiants.

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<span class="mw-page-title-main">1 Camelopardalis</span> Double star system in the constellation Camelopardalis

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<span class="mw-page-title-main">5 Lacertae</span> Star in the constellation Lacerta

5 Lacertae is a spectroscopic binary in the constellation Lacerta. Its apparent magnitude is 4.36.

Tau<sup>1</sup> Lupi Star in the constellation Lupus

Tau1 Lupi, Latinized from τ1 Lupi, is a solitary star in the southern constellation of Lupus. It is visible to the naked eye with an apparent visual magnitude of 4.5. Based upon an annual parallax shift of only 2.99 mas as seen from Earth, it is located about 1,090 light years from the Sun. Tau1 Lupi may be a runaway star having a peculiar velocity of 32.6±3.6 km/s. It is a member of the Upper Centaurus–Lupus sub-group of the nearby Sco OB2 association.

<span class="mw-page-title-main">1 Puppis</span> Star in the constellation Puppis

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<span class="mw-page-title-main">Y Centauri</span> Variable star in the constellation Centaurus

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<span class="mw-page-title-main">16 Lacertae</span> Triple star system in the constellation Lacerta

16 Lacertae is a triple star system in the northern constellation of Lacerta, located about 1,580 light years from the Sun. It has the variable star designation EN Lacertae; 16 Lacertae is the Flamsteed designation. This system is visible to the naked eye as a faint blue-white hued star with a maximum apparent visual magnitude of +5.587. It is moving closer to the Earth with a heliocentric radial velocity of –12 km/s.

<span class="mw-page-title-main">3 Geminorum</span> Star in the constellation Gemini

3 Geminorum is a blue supergiant star in the constellation Gemini. It is a small amplitude pulsating variable and a close double star, with a mean combined apparent visual magnitude of about 5.7.

<span class="mw-page-title-main">V419 Cephei</span> Star in the constellation Cepheus

V419 Cephei is an irregular variable star in the constellation of Cepheus with an apparent magnitude that varies between 6.54 and 6.89.

<span class="mw-page-title-main">NGC 7419</span> Open cluster in the constellation Cepheus

NGC 7419 is an open cluster in the constellation Cepheus. It is heavily reddened and notable for containing five red supergiants, the highest number known in any cluster until the end of the 20th century, but probably no blue supergiants.

<span class="mw-page-title-main">12 Lacertae</span> Star in the constellation Lacerta

12 Lacertae is a wide binary star system in the northern constellation of Lacerta, located roughly 1,260 light years away from the Sun based on parallax. It is visible to the naked eye as a dim, blue-white hued point of light with a baseline apparent visual magnitude of 5.23. The system is drifting closer to the Earth with a mean heliocentric radial velocity of –12.5. It is a probable member of the I Lacertae OB association.

<span class="mw-page-title-main">DH Cephei</span> Binary star system in the constellation Cepheus

DH Cephei is a variable binary star system in the northern circumpolar constellation of Cepheus, positioned about two degrees to the east of the star system Delta Cephei. With an apparent visual magnitude of 8.61, it is too faint to be visible without a telescope. Based on parallax measurements, this system is located at a distance of approximately 9.6 kilolight-years from the Sun. At present it is moving closer to the Earth with a radial velocity of −33 km/s.

References

  1. 1 2 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv: 0708.1752 . Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID   18759600.
  2. 1 2 3 Ducati, J. R. (2002). "VizieR On-line Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  3. 1 2 3 4 U Lac, database entry, The combined table of GCVS Vols I-III and NL 67-78 with improved coordinates, General Catalogue of Variable Stars Archived 2017-06-20 at the Wayback Machine , Sternberg Astronomical Institute, Moscow, Russia. Accessed on line November 12, 2010.
  4. ↑ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID   119231169.
  5. 1 2 3 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  6. ↑ Reiter, Megan; Marengo, Massimo; Hora, Joseph L.; Fazio, Giovanni G. (2015). "A Spitzer/IRAC characterization of Galactic AGB and RSG stars". Monthly Notices of the Royal Astronomical Society. 447 (4): 3909. arXiv: 1501.02749 . Bibcode:2015MNRAS.447.3909R. doi: 10.1093/mnras/stu2725 . S2CID   118515353.
  7. 1 2 Stothers, R.; Leung, K. C. (1971). "Luminosities, masses and periodicities of massive red supergiants". Astronomy and Astrophysics. 10: 290. Bibcode:1971A&A....10..290S.
  8. 1 2 3 Healy, Sarah; Horiuchu, Shunsaku; Colomer Moller, Marta; Milisavljevic, Dan; Tseng, Jeff; Bergin, Faith; Weil, Kathryn; Tanaka, Masaomi (2024). "Red supergiant candidates for multimessenger monitoring of the next Galactic supernova". Monthly Notices of the Royal Astronomical Society. 529 (4): 3630–3650. arXiv: 2307.08785 . Bibcode:2024MNRAS.529.3630H. doi: 10.1093/mnras/stae738 .
  9. ↑ Garmany, C. D.; Stencel, R. E. (1992). "Galactic OB associations in the northern Milky Way Galaxy. I - Longitudes 55 deg to 150 deg". Astronomy and Astrophysics Supplement Series. 94: 211. Bibcode:1992A&AS...94..211G.
  10. ↑ Zejda, M.; Paunzen, E.; Baumann, B.; Mikulášek, Z.; Liška, J. (2012). "Catalogue of variable stars in open cluster fields". Astronomy & Astrophysics. 548: A97. arXiv: 1211.1153 . Bibcode:2012A&A...548A..97Z. doi:10.1051/0004-6361/201219186. S2CID   54789717.
  11. ↑ Burki, G.; Mayor, M. (1983). "Nineteen new spectroscopic binaries and the rate of binary stars among F-M supergiants". Astronomy and Astrophysics. 124: 256. Bibcode:1983A&A...124..256B.
  12. ↑ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
  13. ↑ Espin, T. E. (June 1894). "Stars with remarkable Spectra". Astronomische Nachrichten. 135 (16): 265–274. Bibcode:1894AN....135..265E. doi:10.1002/asna.18941351602 . Retrieved 21 December 2024.
  14. ↑ Blackhouse, T. W. (1902). "The variable star 2.1902 Lacertae". Astronomische Nachrichten. 158 (24): 383–384. doi:10.1002/asna.19021582407 . Retrieved 21 December 2024.
  15. ↑ Cannon, Annie J. (1907). "Second catalogue of variable stars". Annals of Harvard College Observatory. 55: 1–94. Bibcode:1907AnHar..55....1C . Retrieved 18 December 2024.
  16. ↑ Houk, N. (1963). "V1280 Sagttarii and the other long-period variables with secondary period". Astronomical Journal. 68: 253. Bibcode:1963AJ.....68..253H. doi:10.1086/108948.
  17. ↑ Adelman, Saul J. (2001). "Stars with the Largest Hipparcos Photometric Amplitudes". Baltic Astronomy. 10 (4): 589. Bibcode:2001BaltA..10..589A. doi: 10.1515/astro-2001-0403 . S2CID   116386247.
  18. ↑ Yoon, Dong-Hwan; Cho, Se-Hyung; Kim, Jaeheon; Yun, Young joo; Park, Yong-Sun (2014). "SiO and H2O Maser Survey toward Post-asymptotic Giant Branch and Asymptotic Giant Branch Stars". The Astrophysical Journal Supplement. 211 (1): 15. Bibcode:2014ApJS..211...15Y. doi: 10.1088/0067-0049/211/1/15 . S2CID   73561291.
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