LP Andromedae

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LP Andromedae
LPAndLightCurve.png
A near-infrared (L band) light curve for LP Andromedae, adapted from Jones et al. (1990) [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Andromeda
Right ascension 23h 34m 27.5216s [2]
Declination +43° 33′ 01.2996″ [2]
Apparent magnitude  (V)15.12 variable [3]
Characteristics
Spectral type C8,3.5e [4]
Apparent magnitude  (G)16.9041 [2]
Apparent magnitude  (J)9.623 [5]
Apparent magnitude  (H)6.355 [5]
Apparent magnitude  (K)2.71 [6]
Variable type Mira [7]
Astrometry
Proper motion (μ)RA: −21.313±0.532 [2]   mas/yr
Dec.: −22.058±0.453 [2]   mas/yr
Parallax (π)2.5002 ± 0.3626  mas [2]
Distance approx. 1,300  ly
(approx. 400  pc)
Absolute bolometric
magnitude  (Mbol)		−5.21±0.26 [8]
Details [8]
Mass 0.8  M☉
Radius 340 – 420  R☉
Luminosity 2,900 – 16,200  L☉
Temperature 2,100 – 3,350  K
Other designations
2MASS J23342752+4333012, IRAS 23320+4316, RAFGL 3116
Database references
SIMBAD data

LP Andromedae (often abbreviated to LP And) is a carbon star in the constellation Andromeda. It is also a Mira variable [7] whose mean apparent visual magnitude is 15.12 and has pulsations with an amplitude of 1.50 magnitudes [3] and a period of 614 days. [8]

In 1974 LP Andromedae, known then as IRC+40540, was identified as a carbon star and also shown to be variable. [9] It had previously been suspected of variability during the 2 Micron All Sky Survey (2MASS). A detailed study of its spectrum showed an unusually cool star with a basic class of C8, and Swan band strength of 3.5. It also showed strong C13 isotopic bands. [4] The period was narrowed down to around 614 days, one of the longest periods known for a Mira variable. [10]

This star has a dusty envelope with an estimated mass of 3.2 M☉, fueled by the star itself which is losing mass at a rate 1.9×10−5M☉/yr. Such a high mass loss rate should place LP Andromedae close to the end of its asymptotic giant branch evolution. The envelope extends to a distance of 3 parsec from the star, and is mainly made of silicon carbide and carbon particles. [8]

See also

Related Research Articles

<span class="mw-page-title-main">LN Andromedae</span> Star in the constellation Andromeda

LN Andromedae, also known as HD 217811, HR 8768, is a formerly suspected variable star in the constellation Andromeda. Located approximately 458 parsecs (1,490 ly) away from Earth, it shines with an apparent visual magnitude 6.41, thus it can be seen by the naked eye under very favourable conditions. Its spectral classification is B2V, meaning that it's a hot main sequence star, emitting light approximately with a blackbody spectrum at an effective temperature of 18,090 K.

WR 114 is a Wolf-Rayet star in the constellation of Scutum. It is an early type star of the carbon sequence (WCE) classified as WC5.

<span class="mw-page-title-main">IK Tauri</span> Mira variable star in the constellation Taurus

IK Tauri or NML Tauri is a Mira variable star located about 280 parsecs (910 ly) from the Sun in the zodiac constellation of Taurus.

QV Andromedae is an Alpha2 Canum Venaticorum variable in the constellation Andromeda. Its maximum apparent visual magnitude is 6.6, so it can be seen by the naked eye under very favourable conditions. The brightness varies slightly following a periodic cycle of approximately 5.23 days.

<span class="mw-page-title-main">XZ Andromedae</span> Binary star in the constellation Andromeda

XZ Andromedae is a binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 9.91, but drops down to 12.45 every 1.357 days. Its variability matches the behaviour of Algol variable stars.

<span class="mw-page-title-main">AB Andromedae</span> Binary star in the Andromeda constellation

AB Andromedae is a binary star in the constellation Andromeda. Paul Guthnick and Richard Prager discovered that the star is an eclipsing binary in 1927. Its maximum apparent visual magnitude is 9.49 but shows a variation in brightness down to a magnitude of 10.46 in a periodic cycle of roughly 8 hours. The observed variability is typical of W Ursae Majoris variable stars, so the two stars in this system form a contact binary.

<span class="mw-page-title-main">AD Andromedae</span> Eclipsing binary star in the constellation Andromeda

AD Andromedae is an eclipsing binary in the constellation Andromeda. Its maximum apparent visual magnitude is 11.2, but it shows a decrease of 0.62 magnitudes during the main eclipse and 0.58 during the secondary one. It is classified as a Beta Lyrae variable star with a period of almost one day.

<span class="mw-page-title-main">AR Andromedae</span> Star in the constellation Andromeda

AR Andromedae is a dwarf nova of the SS Cygni type in the constellation Andromeda. Its typical apparent visual magnitude is 17.6, but increases up to 11.0 magnitude during outbursts. The outbursts occur approximately every 23 days.

<span class="mw-page-title-main">BM Andromedae</span> Star in the constellation Andromeda

BM Andromedae is a T Tauri star in the constellation Andromeda. Its apparent visual magnitude has irregular variations between a maximum of 11.63 and a minimum of 14.02.

<span class="mw-page-title-main">BX Andromedae</span> Star in the constellation Andromeda

BX Andromedae is an eclipsing binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 8.87. Within a cycle of approximately 14.6 hours, the brightness drops down to a magnitude of 9.53 during the main eclipse, and to a magnitude of 9.12 during the secondary one. It is classified as a Beta Lyrae variable.

<span class="mw-page-title-main">CC Andromedae</span> Star in the constellation Andromeda

CC Andromedae is a variable star in the constellation Andromeda. It is a pulsating star of the Delta Scuti type, with an apparent visual magnitude that varies between 9.19 and 9.46 with a periodicity of 3 hours.

<span class="mw-page-title-main">CN Andromedae</span> Star in the constellation Andromeda

CN Andromedae is an eclipsing binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 9.62 and drops down to a minimum of 10.2 during the main eclipse. It is classified as a Beta Lyrae variable with a period roughly of 0.4628 days.

<span class="mw-page-title-main">EU Andromedae</span> Star in the constellation Andromeda

EU Andromedae is a carbon star in the constellation Andromeda. Its apparent visual magnitude varies in an irregular manner between 10.7 and 11.8.

<span class="mw-page-title-main">FF Andromedae</span> Star in the constellation Andromeda

FF Andromedae is a spectroscopic binary in the constellation Andromeda. It has a typical apparent visual magnitude of 10.4, but undergoes flare events that can increase its brightness by about a magnitude.

<span class="mw-page-title-main">GR Andromedae</span> Variable star in the constellation Andromeda

GR Andromedae is a variable star in the constellation Andromeda. Its apparent visual magnitude varies between 6.87 and 6.95 in a cycle of 518.2 days. It is classified as an α2 Canum Venaticorum variable.

<span class="mw-page-title-main">KX Andromedae</span> Spectroscopic binary star in the constellation Andromeda

KX Andromedae is a spectroscopic binary star in the constellation Andromeda. Its apparent visual magnitude varies between 6.88 and 7.28.

<span class="mw-page-title-main">KZ Andromedae</span> Star in the constellation Andromeda

KZ Andromedae is a double lined spectroscopic binary in the constellation Andromeda. Its apparent visual magnitude varies between 7.91 and 8.03 during a cycle slightly longer than 3 days.

<span class="mw-page-title-main">QR Andromedae</span> Eclipsing binary star in the constellation Andromeda

QR Andromedae is an eclipsing binary star in the constellation Andromeda. Its maximum apparent visual magnitude is 12.16, but its light curve shows clearly eclipsing events where its brightness can drop to a magnitude of 13.07. This leads to its classification as an Algol variable star.

<span class="mw-page-title-main">QX Andromedae</span> Eclipsing binary star system in the constellation Andromeda

QX Andromedae is an eclipsing binary in the constellation Andromeda. It varies from a maximum apparent visual magnitude of 11.28 to a minimum of 11.50. Since it is impossible to specify the onset time of the eclipses, it is classified as a W Ursae Majoris variable star. It is also observed as an X-ray source and is a member of the open cluster NGC 752.

<span class="mw-page-title-main">V455 Andromedae</span> Dwarf nova star in the constellation Andromeda

V455 Andromedae is a dwarf nova in the constellation Andromeda. It has a typical apparent visual magnitude of 16.5, but reached a magnitude of 8.5 during the only observed outburst.

References

  1. ↑ Jones, Terry Jay; Bryja, C. O.; Gehrz, Robert D.; Harrison, Thomas E.; Johnson, Joni J.; Klebe, Dimitri I.; Lawrence, Geoffrey F. (November 1990). "Photometry of Variable AFGL Sources". Astrophysical Journal Supplement. 74: 785. Bibcode:1990ApJS...74..785J. doi: 10.1086/191518 .
  2. 1 2 3 4 5 6 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.
  3. 1 2 Database entry, The Catalina Surveys periodic variable star catalog. (Drake+, 2014), A. J. Drake et al., CDS ID J/ApJS/213/9 Accessed on line 2018-11-14.
  4. 1 2 Cohen, M. (1979). "Circumstellar envelopes and the evolution of carbon stars". Monthly Notices of the Royal Astronomical Society. 186 (4): 837–852. Bibcode:1979MNRAS.186..837C. doi: 10.1093/mnras/186.4.837 .
  5. 1 2 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  6. ↑ Menzies, J. W.; Feast, M. W.; Whitelock, P. A. (June 2006). "Carbon-rich Mira variables: radial velocities and distances". Monthly Notices of the Royal Astronomical Society. 369 (2): 783–790. arXiv: astro-ph/0603505 . Bibcode:2006MNRAS.369..783M. CiteSeerX   10.1.1.255.9712 . doi:10.1111/j.1365-2966.2006.10323.x. S2CID   18684991.
  7. 1 2 N. N. Samus; O. V. Durlevich; et al. "LP And database entry". Combined General Catalog of Variable Stars (2017 ed.). CDS . Retrieved 2018-11-14.
  8. 1 2 3 4 Men'shchikov, A. B.; Balega, Y. Y.; Berger, M.; Driebe, T.; Hofmann, K.-H.; Maximov, A. F.; Schertl, D.; Shenavrin, V. I.; Weigelt, G. (March 2006). "Near-infrared speckle interferometry and radiative transfer modelling of the carbon star LP Andromedae". Astronomy and Astrophysics. 448 (1): 271–281. Bibcode:2006A&A...448..271M. doi: 10.1051/0004-6361:20052976 .
  9. ↑ Lockwood, G. W. (1974). "Near-infrared photometry of unidentified IRC stars. II". The Astrophysical Journal. 192: 113. Bibcode:1974ApJ...192..113L. doi: 10.1086/153041 .
  10. ↑ Alksnis, A. (1989). "On the Variability of the Dusty Carbon Star LP and". Information Bulletin on Variable Stars. 3396: 1. Bibcode:1989IBVS.3396....1A.
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