Langbahn Team – Weltmeisterschaft

Kepler-411

Kepler-411
Observation data
Epoch J2000      Equinox J2000
Constellation Cygnus
Right ascension 19h 10m 25.34699s[1]
Declination +49° 31′ 23.7126″[1]
Apparent magnitude (V) 12.55[2]
Characteristics
Kepler-411A
Evolutionary stage main-sequence star
Spectral type K3V
Astrometry
Kepler-411A
Radial velocity (Rv)−20.40±0.77[1] km/s
Proper motion (μ) RA: 13.611[1] mas/yr
Dec.: 32.543[1] mas/yr
Parallax (π)6.5313 ± 0.0080 mas[3]
Distance499.4 ± 0.6 ly
(153.1 ± 0.2 pc)
Kepler-411B
Proper motion (μ) RA: 13.263[3] mas/yr
Dec.: 33.008[3] mas/yr
Parallax (π)6.5727 ± 0.0573 mas[3]
Distance496 ± 4 ly
(152 ± 1 pc)
Position (relative to Kepler-411A)[4]
ComponentKepler-411B
Epoch of observation2012
Angular distance3.4±0.06″
Position angle331±3°
Projected separation520 AU
Details
Kepler-411A
Mass0.75[1] M☉
Radius0.76[1] R☉
Luminosity0.27[1] L☉
Surface gravity (log g)4.58[1] cgs
Temperature4,773[1] K
Metallicity [Fe/H]0.11±0.1[5] dex
Rotation10.52 d[6]
Age0.212±0.031[7] Gyr
Kepler-411B
Mass0.33[8] M☉
Radius0.49[4] R☉
Temperature3,446[8] K
Other designations
Kepler-411A: KOI-1781, KIC 11551692, 2MASS J19102533+4931237[2]
Kepler-411B: Gaia DR3 2132768956904826624
Database references
SIMBADdata

Kepler-411 is a binary star system. Its primary star Kepler-411A is a K-type main-sequence star, orbited by the red dwarf star Kepler-411B on a wide orbit, discovered in 2012.[4]

Primary star

The primary star's surface temperature is 4,773 K. Kepler-411A is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of 0.11±0.1,[5] but is much younger at an age of 212±31 million years.[7]

Kepler-411A exhibits significant starspot activity, with starspots covering 1.7+0.3
−0.2% of the stellar surface.[9] Darker starspots are concentrated around the equator of the star. Kepler-411A exhibits differential rotation, but with smaller amount of differential shear compared to the Sun.[6]

The companion Kepler-411B is 533 au away from Kepler-411A.[8] It is a red dwarf and a flare star.[10]

Planetary system

In 2013, one planet, named Kepler-411b, was discovered,[11] followed by planet Kepler-411c in 2016. Third planet in system detected by transit method, d, along with e detected by radial velocity method, were discovered in 2019.[12][7]


The Kepler-411 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b[13] 0.08055±0.00818 MJ 0.0375±0.0008 3.005156±0.000002 0.146+0.004
−0.005 		87.4±0.1° 0.214±0.005 RJ
c[14] 0.08306±0.01856 MJ 0.0739±0.001 7.834436247±0.000001137[15] 0.108+0.003
−0.004 		88.61±0.04° 0.394±0.006 RJ
d[16] 0.04782±0.01605 MJ 0.279±0.004 58.02023116±0.00004203[15] 0.128±0.003 89.43±0.02° 0.296±0.009 RJ
e[17] 0.03398±0.00346 MJ 0.186±0.003 31.509728±0.000085 0.016+0.002
−0.001 		88.04±0.02° —

References

  1. ^ a b c d e f g h i j 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 "Kepler-411". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-02-22.
  3. ^ a b c d 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 Ziegler, Carl; Law, Nicholas M.; Baranec, Christoph; Riddle, Reed; Duev, Dmitry A.; Howard, Ward; Jensen-Clem, Rebecca; Kulkarni, S. R.; Morton, Tim; Salama, Maïssa (2017), "Robo-AO Kepler survey. IV. The effect of nearby stars on 3857 planetary candidate systems", The Astronomical Journal, 155 (4): 161, arXiv:1712.04454, doi:10.3847/1538-3881/aab042, S2CID 119088873
  5. ^ a b Furlan, E.; Ciardi, D. R.; Cochran, W. D.; Everett, M. E.; Latham, D. W.; Marcy, G. W.; Buchhave, L. A.; Endl, M.; Isaacson, H.; Petigura, E. A.; Gautier, T. N.; Huber, D.; Bieryla, A.; Borucki, W. J.; Brugamyer, E.; Caldwell, C.; Cochran, A.; Howard, A. W.; Howell, S. B.; Johnson, M. C.; MacQueen, P. J.; Quinn, S. N.; Robertson, P.; Mathur, S.; Batalha, N. M. (2018), "The Kepler Follow-Up Observation Program. II. Stellar Parameters from Medium- and High-Resolution Spectroscopy", The Astrophysical Journal, 861 (2): 149, arXiv:1805.12089, Bibcode:2018ApJ...861..149F, doi:10.3847/1538-4357/aaca34, S2CID 119243987
  6. ^ a b Araújo, Alexandre; Valio, Adriana (2021), "Kepler-411 differential rotation from three transiting planets", The Astrophysical Journal, 907 (1): L5, arXiv:2101.07692, Bibcode:2021ApJ...907L...5A, doi:10.3847/2041-8213/abd3a7, S2CID 231639459
  7. ^ a b c Lillo-Box, J.; Lopez, T. A.; Santerne, A.; Nielsen, L. D.; Barros, S. C. C.; Deleuil, M.; Acuña, L.; Mousis, O.; Sousa, S. G.; Adibekyan, V.; Armstrong, D. J.; Barrado, D.; Bayliss, D.; Brown, D. J. A.; Demangeon, O. D. S.; Dumusque, X.; Figueira, P.; Hojjatpanah, S.; Osborn, H. P.; Santos, N. C.; Udry, S. (2020), "Masses for the seven planets in K2-32 and K2-233. Four diverse planets in resonant chain and the first young rocky worlds", Astronomy & Astrophysics, A48: 640, arXiv:2006.01102, Bibcode:2020A&A...640A..48L, doi:10.1051/0004-6361/202037896, S2CID 219176756
  8. ^ a b c Mugrauer, M. (2019). "Search for stellar companions of exoplanet host stars by exploring the second ESA-Gaia data release". Monthly Notices of the Royal Astronomical Society. 490 (4): 5088. Bibcode:2019MNRAS.490.5088M. doi:10.1093/mnras/stz2673.
  9. ^ Morris, Brett M. (2020), "A relationship between stellar age and spot coverage", The Astrophysical Journal, 893 (1): 67, arXiv:2002.09135, Bibcode:2020ApJ...893...67M, doi:10.3847/1538-4357/ab79a0, S2CID 211252547
  10. ^ Jackman, James A. G.; Shkolnik, Evgenya; Loyd, R. O. Parke (2021). "Stellar flares from blended and neighbouring stars in Kepler short cadence observations". Monthly Notices of the Royal Astronomical Society. 502 (2): 2033. arXiv:2101.07269. Bibcode:2021MNRAS.502.2033J. doi:10.1093/mnras/stab166.
  11. ^ Wang, Ji; Xie, Ji-Wei; Barclay, Thomas; Fischer, Debra A. (2013), "Influence of Stellar Multiplicity On Planet Formation. I. Evidence of Suppressed Planet Formation Due to Stellar Companions Within 20 AU and Validation of Four Planets From the Kepler Multiple Planet Candidates", The Astrophysical Journal, 783 (1): 4, arXiv:1309.7097, Bibcode:2014ApJ...783....4W, doi:10.1088/0004-637X/783/1/4, S2CID 119214390
  12. ^ Sun, L.; Ioannidis, P.; Gu, S.; Schmitt, J. H. M. M.; Wang, X.; Kouwenhoven, M. B. N. (2019), "Kepler-411: a four-planet system with an active host star", Astronomy & Astrophysics, 624: A15, arXiv:1902.09719, Bibcode:2019A&A...624A..15S, doi:10.1051/0004-6361/201834275, S2CID 102481339
  13. ^ "The Extrasolar Planet Encyclopaedia — Kepler-411 b". Extrasolar Planets Encyclopaedia. Retrieved 2022-09-27.
  14. ^ "The Extrasolar Planet Encyclopaedia — Kepler-411 c". Extrasolar Planets Encyclopaedia. Retrieved 2022-09-27.
  15. ^ a b Battley, Matthew P; et al. (10 March 2021). "Revisiting the Kepler field with TESS: Improved ephemerides using TESS 2 min data". Monthly Notices of the Royal Astronomical Society. 503 (3): 4092–4104. arXiv:2103.03259. Bibcode:2021MNRAS.503.4092B. doi:10.1093/mnras/stab701.
  16. ^ "The Extrasolar Planet Encyclopaedia — Kepler-411 d". Extrasolar Planets Encyclopaedia. Retrieved 2022-09-27.
  17. ^ "The Extrasolar Planet Encyclopaedia — Kepler-411 e". Extrasolar Planets Encyclopaedia. Retrieved 2022-09-27.


Quelle: http://en.wikipedia.org/wiki/Kepler-411