LL Pegasi

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Double star
CRL 3068 / AFGL 3068 / LL Pegasi
Near infrared image from the Hubble Space Telescope. The bright object on the right is a star in the foreground that served as a guiding star for later examination by the larger Keck telescope.
Near infrared image from the Hubble Space Telescope . The bright object on the right is a star in the foreground that served as a guiding star for later examination by the larger Keck telescope.
AladinLite
Observation
dates equinox :  J2000.0 , epoch : J2000.0
Constellation Pegasus
Right ascension 23 h 19 m 12.61 s
declination + 17 ° 11 ′ 33.1 ″
Typing
Spectral class C.
Variable star type M. 
Astrometry
distance (1,300)  pc  
Visual absolute brightness M vis (−5.35) mag
Proper movement 
Rec. Share: (−5.69 ± 0.8)  mas / a
Dec. portion: (−8.22 ± 0.8)  mas / a
Physical Properties
radius (600 to 900)  R ☉
Luminosity

(11000)  L ☉

Effective temperature (2000)  K.
Other names
and catalog entries
2MASS catalog 2MASS J23191260 + 1711331 [1]
Other names LL Pegasi, IRAS 23166 + 1655, RAFGL 3068

CRL 3068 / AFGL 3068 / LL Pegasi is a binary star system surrounded by a spiral nebula in the constellation Pegasus . The two stars were identified through observations from the Keck Observatory . Their apparent distance is 0.11 ″. The cause of the spiral structure is assumed to be the matter emission of one of the two stars (a carbon star ), which is modulated by the mutual orbiting. An orbital period of 710 years was calculated based on the spiral distance and the outflow velocity.

Since both stars are covered by a cloud of dust that is only permeable in the infrared and could not be separated when creating the IRAS directory due to the small distance, they are listed there with a common designation and position.

Spiral structure by LL Pegasi. Composite recording of Hubble and ALMA .

Web links

Commons : LL Pegasi  - collection of images, videos and audio files

Individual evidence

  1. ↑ a b RAFGL 3068. In: SIMBAD . Center de Données astronomiques de Strasbourg , accessed September 9, 2018 .
  2. ↑ a b LL Peg. In: VSX. AAVSO, accessed September 9, 2018 .
  3. ↑ a b c R. Lombaert, BL De Vries, A. De Koter, L. Decin, M. Min, K. Smolders, H. Mutschke, LBFM Waters: Observational evidence for composite grains in an AGB outflow. MgS in the extreme carbon star LL Pegasi . In: Astronomy & Astrophysics . 544, 2012, p. L18. arxiv : 1207.1606 . bibcode : 2012A & A ... 544L..18L . doi : 10.1051 / 0004-6361 / 201219782 .
  4. ↑ Guandalini, R., Cristallo, S .: Luminosities of carbon-rich asymptotic giant branch stars in the Milky Way . In: Astronomy & Astrophysics . 555, 2013, p. 7. arxiv : 1305.4203 . A120. bibcode : 2013A & A ... 555A.120G . doi : 10.1051 / 0004-6361 / 201321225 .
  5. ^ A b c E. De Beck, L. Decin, A. De Koter, K. Justtanont, T. Verhoelst, F. Kemper, KM Menten: Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles . II. CO line survey of evolved stars: Derivation of mass-loss rate formulas . In: Astronomy and Astrophysics . 523, 2010, p. A18. arxiv : 1008.1083 . bibcode : 2010A & A ... 523A..18D . doi : 10.1051 / 0004-6361 / 200913771 .
  6. ↑ Mark Morris, Raghvendra Sahai, Keith Matthews, Judy Cheng, Jessica Lu, Mark Claussen, Carmen Sánchez-Contreras: A Binary-Induced Pinwheel Outflow from the Extreme Carbon Star, AFGL 3068 (PDF; 145 kB)