維基百科

Groombridge 1618

格龍布里奇 1618是位於大熊座的一顆恆星。它的視星等為+6.6，處於或低於普通觀察者肉眼可見恆星的閾值。它距離地球相對較近，距離為15.89光年（4.87光年）。這是一顆光譜類型為K7.5 Ve的主序星，質量僅為太陽的67% 。

Groombridge 1618
Groombridge 1618 is located in the constellation Ursa Major.
Groombridge 1618 is located in the constellation Ursa Major.
Groombridge 1618
Groombridge 1618在大熊座的位置

觀測資料
曆元 J2000.0
星座 大熊座
星官
赤經 10h 11m 22.13995s[1]
赤緯 +49° 27′ 15.2510″[1]
視星等（V） +6.60[2]
特性
光譜分類K7.5 Ve[3]
U−B 色指數+1.27[2]
B−V 色指數+1.34[2]
變星類型BY Dra,[4] Flare star[5]
天體測定
徑向速度 (Rv)−26.48±0.12[1] km/s
自行 (μ) 赤經：−1363.287±0.016 mas/yr
赤緯：−505.770±0.020 mas/yr
視差 (π)205.3148 ± 0.0224[1] mas
距離15.886 ± 0.002 ly
(4.8706 ± 0.0005 pc)
絕對星等 (MV)8.11[6]
詳細資料
質量0.670±0.033[7] M☉
半徑0.605±0.02[7] R☉
表面重力 (log g)4.51;[8] 4.70[7]
亮度 (bolometric)0.15[9] L☉
亮度 (visual, LV)0.049 L☉
溫度3,970[8] K
金屬量 [Fe/H]–0.03[8] dex
自轉速度 (v sin i)2.8[10] km/s
年齡6.6[9] Gyr
其他命名
BD+50° 1725、​GJ 380、​HD 88230、​HIP 49908、​SAO 43223、​LFT 696、​IRAS 10082+4942[11]
參考資料庫
SIMBAD資料

特性

Stephen Groombridge（英語：Stephen Groombridge）

格龍布里奇 1618的恆星分類為K8V，這意味著它是一顆K型主序星，通過在其核心聚變氫來產生能量。它的質量是太陽的67%，半徑是太陽的61%，[7] 但輻射的能量只有太陽的15%，可見光光譜中的能量也只有太陽的 4.6% 。恆星光球層的有效表面溫度約為 4,000 K，呈現橙色。

它也是磁場強度為 750 G 的天龍座BY型變星[4]。色球相對不活躍[12] 並產生可與太陽耀斑媲美的星斑。然而，像UV Ceti一樣，它已被觀察到作為耀星經歷了光度的增加。a[5]

行星搜索

紅外空間天文台對這顆恆星的過量紅外輻射的搜索結果是否定的，這意味著格龍布里奇 1618附近沒有碎片盤（例如織女星）。[13] 然而，使用赫雪爾太空望遠鏡進行的觀測顯示存在低溫碎片盤。數據可以用溫度低於 22 K 的粗糙、高反射性塵埃環模擬，環繞主恆星至少51個天文單位。[9] 如果這顆星確實有伴星，天體測量測量結果似乎將 3-12 倍木星質量的上限置於這樣一個假設的物體上（軌道周期在 5-50 年的範圍內）。[14]

觀測結果傾向於將周期為 122天的單個顯著物體作為行星物體，其最小質量是木星的 4 倍。這顆候選行星從未得到證實，作者發現的信號可能是由於恆星年輕時的內在恆星活動。如果得到證實，這顆行星將位於恆星的宜居帶內。[15] [note 1]

2010 年使用配備自適應光學系統的多鏡面望遠鏡對該系統進行的檢查未能檢測到行星伴星。[17]

這顆恆星的宜居帶定義為類地行星上可能存在液態水的區域，半徑為0.26–0.56個天文單位，其中1個天文單位是地球到太陽的平均距離。[18]

根據美國宇航局戈達德太空飛行中心的分析，這顆恆星是附近五顆K型恆星之一，屬於類太陽恆星和M型恆星之間演化生命可能性的「最佳點」。[19]

參見

注釋

  1. ^   [16] when used to calculate the stellar flux reaching the outer atmosphere of an Earth-like planet orbiting Groombridge 1618 at the Inner Habitable Zone edge - the Runaway Greenhouse limit gives a   of 0.9397 or 93.97% the stellar flux reaching the top of Earth's atmosphere. By applying the previously calculated stellar flux and the known 15% luminosity of Groombridge 1618 into the equation,  ,[16] the distance of the Inner HZ - Runaway Greenhouse limit from Groombridge 1618 can be calculated as  .

參考資料

  1. ^ 1.0 1.1 1.2 1.3 Vallenari, A.; et al. Gaia Data Release 3. Summary of the content and survey properties. Astronomy & Astrophysics. 2022. arXiv:2208.00211  . doi:10.1051/0004-6361/202243940  .  已忽略未知參數|collaboration= (幫助) Gaia DR3 record for this source at VizieR.
  2. ^ 2.0 2.1 2.2 Argue, A. N., UBV photometry of 550 F, G and K type stars, Monthly Notices of the Royal Astronomical Society, 1966, 133 (4): 475–493, Bibcode:1966MNRAS.133..475A, doi:10.1093/mnras/133.4.475   
  3. ^ Lépine, Sébastien; et al, A Spectroscopic Catalog of the Brightest (J < 9) M Dwarfs in the Northern Sky, The Astronomical Journal, 2013, 145 (4): 102, Bibcode:2013AJ....145..102L, S2CID 117144290, arXiv:1206.5991  , doi:10.1088/0004-6256/145/4/102. 
  4. ^ 4.0 4.1 Gudel, M., Radio and X-ray emission from main-sequence K stars, Astronomy and Astrophysics, October 1992, 264 (2): L31–L34, Bibcode:1992A&A...264L..31G. 
  5. ^ 5.0 5.1 Andrillat, Y.; Morguleff, N., Hack, Margherita , 編, Three potassium-flare stars, Proceedings of the Colloquium, held in Trieste, June 13–17, 1966, Trieste, 1967: 160, Bibcode:1967lts..conf..160A. 
  6. ^ Holmberg, J.; et al, The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics, Astronomy and Astrophysics, July 2009, 501 (3): 941–947, Bibcode:2009A&A...501..941H, S2CID 118577511, arXiv:0811.3982  , doi:10.1051/0004-6361/200811191. 
  7. ^ 7.0 7.1 7.2 7.3 Ségransan, Damien; Kervella, Pierre; Forveille, Thierry; Queloz, Didier. First radius measurements of very low mass stars with the VLTI. Astronomy and Astrophysics. 2003, 397 (3): L5–L8. Bibcode:2003A&A...397L...5S. S2CID 10748478. arXiv:astro-ph/0211647  . doi:10.1051/0004-6361:20021714. 
  8. ^ 8.0 8.1 8.2 Woolf, Vincent M.; Wallerstein, George. Metallicity measurements using atomic lines in M and K dwarf stars. Monthly Notices of the Royal Astronomical Society. January 2005, 356 (3): 963–968. Bibcode:2005MNRAS.356..963W. S2CID 15664454. arXiv:astro-ph/0410452  . doi:10.1111/j.1365-2966.2004.08515.x.  See table 3.
  9. ^ 9.0 9.1 9.2 Eiroa, C.; et al, Herschel discovery of a new class of cold, faint debris discs, Astronomy & Astrophysics, December 2011, 536: L4, Bibcode:2011A&A...536L...4E, S2CID 14234038, arXiv:1110.4826  , doi:10.1051/0004-6361/201117797. 
  10. ^ López-Morales, Mercedes. On the Correlation between the Magnetic Activity Levels, Metallicities, and Radii of Low-Mass Stars. The Astrophysical Journal. May 2007, 660 (1): 732–739. Bibcode:2007ApJ...660..732L. S2CID 119530297. arXiv:astro-ph/0701702  . doi:10.1086/513142. 
  11. ^ NSV 4765 -- Flare Star. SIMBAD. Centre de Données astronomiques de Strasbourg. [2013-08-01]. （原始內容存檔於2022-12-05）. 
  12. ^ Byrne, P. B.; Doyle, J. G., Activity in late-type stars. VII - Chromospheric and transition region line fluxes in 2 dM and 1 dM(e) stars, Astronomy and Astrophysics, November 1990, 238 (1–2): 221–226, Bibcode:1990A&A...238..221B. 
  13. ^ Laureijs, R. J.; et al. A 25 micron search for Vega-like disks around main-sequence stars with ISO (PDF). Astronomy & Astrophysics. 2002, 387 (1): L285–L293 [2023-03-20]. Bibcode:2002A&A...387..285L. doi:10.1051/0004-6361:20020366  . hdl:1887/7333. （原始內容存檔 (PDF)於2017-08-09）. 
  14. ^ Hershey, J. L.; Borgman, E. R. Upper Limits on the Mass of a Dark Companion of Groombridge 1618 from the 40-year Sproul Plate Series. Bulletin of the American Astronomical Society. 1978, 10: 630. Bibcode:1978BAAS...10..630H. 
  15. ^ Marcy, Geoffrey W.; Benitz, Karsten J. A search for substellar companions to low-mass stars. Astrophysical Journal, Part 1. 1989, 344 (1): 441–453. Bibcode:1989ApJ...344..441M. doi:10.1086/167812. 
  16. ^ 16.0 16.1 Kopparapu, R. K.; Ramirez, R.; Kasting, J.F.; Eymet, V.; Robinson, T. D.; Mahadevan, S.; Terrien, R.C.; Domagal-Goldman, S.; Meadows, R.; Deshpande, V. Habitable Zones around Main-sequence Stars: New Estimates. The Astrophysical Journal. March 2013, 765 (2): 16. Bibcode:2013ApJ...765..131K. S2CID 76651902. arXiv:1301.6674  . doi:10.1088/0004-637X/765/2/131. 
  17. ^ Heinze, A. N.; et al. Constraints on Long-period Planets from an L'- and M-band Survey of Nearby Sun-like Stars: Observations. The Astrophysical Journal. May 2010, 714 (2): 1551–1569. Bibcode:2010ApJ...714.1551H. S2CID 119199321. arXiv:1003.5340  . doi:10.1088/0004-637X/714/2/1551. 
  18. ^ Cantrell, Justin R.; et al, The Solar Neighborhood XXIX: The Habitable Real Estate of Our Nearest Stellar Neighbors, The Astronomical Journal, October 2013, 146 (4): 99, Bibcode:2013AJ....146...99C, S2CID 44208180, arXiv:1307.7038  , doi:10.1088/0004-6256/146/4/99. 
  19. ^ Bill Steigerwald. "Goldilocks" Stars May Be "Just Right" for Finding Habitable Worlds. NASA. 2019-03-07 [2020-05-12]. （原始內容存檔於2019-06-17）. 'I find that certain nearby K stars like 61 Cyg A/B, Epsilon Indi, Groombridge 1618, and HD 156026 may be particularly good targets for future biosignature searches,' said Arney. 

註釋

外部連結

取自「https://zh.wikipedia.org/w/index.php?title=Groombridge_1618&oldid=83166818」