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LL Pegasi (AFGL 3068) is a Mira variable star surrounded by a pinwheel-shaped nebula, IRAS 23166+1655, thought to be a preplanetary nebula. It is a binary system that includes an extreme carbon star. The pair is hidden by the dust cloud ejected from the carbon star and is only visible in infrared light.[7]

LL Pegasi

LL Pegasi is continuously losing gaseous material as it evolves into a planetary nebula.[1]
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Pegasus
Right ascension 23h 19m 12.607s[2]
Declination +17° 11′ 33.13″[2]
Characteristics
Evolutionary stage Asymptotic giant branch[3]
Spectral type C[4]
Variable type Mira[5]
Astrometry
Distance1,300[3] pc
Details
Radius1,074[6] R☉
Luminosity10,900[6] L☉
Temperature1,800[6] K
Other designations
LL Pegasi, IRAS 23166+1655, 2MASS J23191260+1711331, RAFGL 3068
Database references
SIMBADdata

Variability


A near-infrared (L- band) light curve for LL Pegasi, plotted from data published by Le Bertre (1992)[8]
A near-infrared (L- band) light curve for LL Pegasi, plotted from data published by Le Bertre (1992)[8]

LL Pegasi is obscured at visual wavelengths, but is strongly variable in brightness at infrared wavelengths.[8] It is classified as a Mira variable and has a period of about 696 days.[9]


Nebula


The nebula displays an unusual Archimedean spiral shape. The shape is thought to be formed through the interaction between the stellar companion and the carbon star, as has been seen in other binary systems, although not with such a precise geometric form. The distance between the spiral arms and their rate of expansion is consistent with estimates of the pair's 810 year orbital period based on their apparent angular separation.[7]




References


  1. "Celestial spiral with a twist". eso.org. European Southern Observatory. Retrieved 13 February 2022.
  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.
  3. Lombaert, R.; De Vries, B. L.; De Koter, A.; Decin, L.; Min, M.; Smolders, K.; Mutschke, H.; Waters, L. B. F. M. (2012). "Observational evidence for composite grains in an AGB outflow. MgS in the extreme carbon star LL Pegasi". Astronomy & Astrophysics. 544: L18. arXiv:1207.1606. Bibcode:2012A&A...544L..18L. doi:10.1051/0004-6361/201219782. S2CID 119022145.
  4. Groenewegen, M. A. T.; De Jong, T.; Gaballe, T. R. (1994). "The 3 micrometer spectra of candidate carbon stars". Astronomy and Astrophysics. 287: 163. Bibcode:1994A&A...287..163G.
  5. Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  6. Massalkhi, S.; Agúndez, M.; Cernicharo, J. (August 2019). "Study of CS, SiO, and SiS abundances in carbon star envelopes: Assessing their role as gas-phase precursors of dust". Astronomy & Astrophysics. 628: A62. arXiv:1906.09461. doi:10.1051/0004-6361/201935069. ISSN 0004-6361.
  7. Morris, Mark; Sahai, Raghvendra; Matthews, Keith; Cheng, Judy; Lu, Jessica; Claussen, Mark; Sánchez-Contreras, Carmen (2006). "A Binary-Induced Pinwheel Outflow from the Extreme Carbon Star, AFGL 3068". Planetary Nebulae in Our Galaxy and Beyond. 234: 469. Bibcode:2006IAUS..234..469M. doi:10.1017/S1743921306003784.
  8. Le Bertre, T. (1992). "Carbon-star lightcurves in the 1-20 micron range". Astronomy and Astrophysics Supplement Series. 94: 377. Bibcode:1992A&AS...94..377L.
  9. Whitelock, Patricia A.; Feast, Michael W.; Marang, Freddy; Groenewegen, M. A. T. (2006). "Near-infrared photometry of carbon stars". Monthly Notices of the Royal Astronomical Society. 369 (2): 751–782. arXiv:astro-ph/0603504. Bibcode:2006MNRAS.369..751W. doi:10.1111/j.1365-2966.2006.10322.x. S2CID 14453496.



На других языках

[de] LL Pegasi

CRL 3068 / AFGL 3068 / LL Pegasi ist ein von einem spiralförmigen Nebel umgebenes Doppelsternsystem im Sternbild Pegasus. Die beiden Sterne wurden durch Beobachtungen des Keck-Observatoriums ermittelt. Ihr scheinbarer Abstand beträgt 0,11″. Als Ursache für die Spiralstruktur wird die Materieemission eines der beiden Sterne (ein Kohlenstoffstern) angenommen, die durch das gegenseitige Umkreisen moduliert wird. Anhand des Spiralabstands und der Ausströmgeschwindigkeit wurde eine Umlaufzeit von 710 Jahren errechnet.[6]
- [en] LL Pegasi

[it] LL Pegasi

LL Pegasi (LL Peg) è una stella variabile di tipo Mira osservabile nella costellazione di Pegaso, distante approssimativamente tra 3420 (1050 pc[3]) e 4240 anni luce (1300 pc[4]) dal sistema solare.

[ru] IRAS 23166+1655

IRAS 23166+1655 является протопланетарной туманностью, окружающей LL Пегаса (также имеющей обозначение AFGL 3068) — двойную систему, которая включает в себя углеродную звезду. Пара скрыта облаком пыли, выбрасываемым с поверхности углеродной звезды, и видна только в инфракрасном свете[1].


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