Groombridge 1618

**Groombridge 1618**
	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
光谱分类	K7.5 Ve[3]
U−B 色指数	+1.27[2]
B−V 色指数	+1.34[2]
变星类型	BY Dra,[4] Flare star[5]
天体测定
徑向速度 (Rv)	−26.48±0.12[1] km/s
自行 (μ)	赤经：−1363.287±0.016 mas/yr ; 赤纬：−505.770±0.020 mas/yr
视差 (π)	205.3148 ± 0.0224[1] mas
距离	15.886 ± 0.002 ly ; (4.8706 ± 0.0005 pc)
绝对星等 (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
金属量 [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	资料

格龙布里奇 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% 。

特性

Stephen Groombridge

格龙布里奇 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，這意味著格龙布里奇 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

鄰近恆星列表

注釋

$\scriptstyle S_{eff_{\ast }}=S_{eff_{\odot }}+aT_{\ast }+bT_{\ast }^{2}+cT_{\ast }^{3}+dT_{\ast }^{4}$ [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 $\scriptstyle S_{eff_{\ast }}$ 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, $\scriptstyle {d={\left({\frac {{L_{\ast }}/{L_{\odot }}}{S_{eff_{\ast }}}}\right)^{0.5}AU}}$ ,[16] the distance of the Inner HZ - Runaway Greenhouse limit from Groombridge 1618 can be calculated as $\scriptstyle {0.4AU}$ .

參考資料

Vallenari, A.; et al. . Astronomy & Astrophysics. 2022. arXiv:2208.00211 . doi:10.1051/0004-6361/202243940 . 已忽略未知参数|collaboration= (帮助) Gaia DR3 record for this source at VizieR.
Argue, A. N., , Monthly Notices of the Royal Astronomical Society, 1966, 133 (4): 475–493, Bibcode:1966MNRAS.133..475A, doi:10.1093/mnras/133.4.475 
Lépine, Sébastien; et al, , The Astronomical Journal, 2013, 145 (4): 102, Bibcode:2013AJ....145..102L, S2CID 117144290, arXiv:1206.5991 , doi:10.1088/0004-6256/145/4/102.
Gudel, M., , Astronomy and Astrophysics, October 1992, 264 (2): L31–L34, Bibcode:1992A&A...264L..31G.
Andrillat, Y.; Morguleff, N., Hack, Margherita , 编, , Proceedings of the Colloquium, held in Trieste, June 13–17, 1966, Trieste, 1967: 160, Bibcode:1967lts..conf..160A.
Holmberg, J.; et al, , 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.
Ségransan, Damien; Kervella, Pierre; Forveille, Thierry; Queloz, Didier. . 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.
Woolf, Vincent M.; Wallerstein, George. . 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.
Eiroa, C.; et al, , Astronomy & Astrophysics, December 2011, 536: L4, Bibcode:2011A&A...536L...4E, S2CID 14234038, arXiv:1110.4826 , doi:10.1051/0004-6361/201117797.
López-Morales, Mercedes. . The Astrophysical Journal. May 2007, 660 (1): 732–739. Bibcode:2007ApJ...660..732L. S2CID 119530297. arXiv:astro-ph/0701702 . doi:10.1086/513142.
. SIMBAD. Centre de Données astronomiques de Strasbourg. [2013-08-01]. （原始内容存档于2022-12-05）.
Byrne, P. B.; Doyle, J. G., , Astronomy and Astrophysics, November 1990, 238 (1–2): 221–226, Bibcode:1990A&A...238..221B.
Laureijs, R. J.; et al. (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. （原始内容存档 (PDF)于2017-08-09）.
Hershey, J. L.; Borgman, E. R. . Bulletin of the American Astronomical Society. 1978, 10: 630. Bibcode:1978BAAS...10..630H.
Marcy, Geoffrey W.; Benitz, Karsten J. . Astrophysical Journal, Part 1. 1989, 344 (1): 441–453. Bibcode:1989ApJ...344..441M. doi:10.1086/167812.
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. . 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.
Heinze, A. N.; et al. . 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.
Cantrell, Justin R.; et al, , 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.
Bill Steigerwald. . NASA. 2019-03-07 [2020-05-12]. （原始内容存档于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

. Sol Company. [2007-06-24]. （原始内容存档于2012-05-11）.
. Astronomisches Rechen-Institut. [2007-06-24]. （原始内容存档于2007-06-10）.

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[maximum_greenhouse-17] $\scriptstyle S_{eff_{\ast }}=S_{eff_{\odot }}+aT_{\ast }+bT_{\ast }^{2}+cT_{\ast }^{3}+dT_{\ast }^{4}$ [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 $\scriptstyle S_{eff_{\ast }}$ 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, $\scriptstyle {d={\left({\frac {{L_{\ast }}/{L_{\odot }}}{S_{eff_{\ast }}}}\right)^{0.5}AU}}$ ,[16] the distance of the Inner HZ - Runaway Greenhouse limit from Groombridge 1618 can be calculated as $\scriptstyle {0.4AU}$ .

[GaiaDR3-1] Vallenari, A.; et al. . Astronomy & Astrophysics. 2022. arXiv:2208.00211 . doi:10.1051/0004-6361/202243940 . 已忽略未知参数|collaboration= (帮助) Gaia DR3 record for this source at VizieR.

[mnras133_475-2] Argue, A. N., , Monthly Notices of the Royal Astronomical Society, 1966, 133 (4): 475–493, Bibcode:1966MNRAS.133..475A, doi:10.1093/mnras/133.4.475 

[lepine2013-3] Lépine, Sébastien; et al, , The Astronomical Journal, 2013, 145 (4): 102, Bibcode:2013AJ....145..102L, S2CID 117144290, arXiv:1206.5991 , doi:10.1088/0004-6256/145/4/102.

[AAA264_2_L31-4] Gudel, M., , Astronomy and Astrophysics, October 1992, 264 (2): L31–L34, Bibcode:1992A&A...264L..31G.

[Andrillat_Morguleff-5] Andrillat, Y.; Morguleff, N., Hack, Margherita , 编, , Proceedings of the Colloquium, held in Trieste, June 13–17, 1966, Trieste, 1967: 160, Bibcode:1967lts..conf..160A.

[cgssn09-6] Holmberg, J.; et al, , 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.

[aaa397_L5-7] Ségransan, Damien; Kervella, Pierre; Forveille, Thierry; Queloz, Didier. . 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.

[mnras356-8] Woolf, Vincent M.; Wallerstein, George. . 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.

[AAA536_L4-9] Eiroa, C.; et al, , Astronomy & Astrophysics, December 2011, 536: L4, Bibcode:2011A&A...536L...4E, S2CID 14234038, arXiv:1110.4826 , doi:10.1051/0004-6361/201117797.

[apj660_1_732-10] López-Morales, Mercedes. . The Astrophysical Journal. May 2007, 660 (1): 732–739. Bibcode:2007ApJ...660..732L. S2CID 119530297. arXiv:astro-ph/0701702 . doi:10.1086/513142.

[SIMBAD-11] . SIMBAD. Centre de Données astronomiques de Strasbourg. [2013-08-01]. （原始内容存档于2022-12-05）.

[AAA238_1_221-12] Byrne, P. B.; Doyle, J. G., , Astronomy and Astrophysics, November 1990, 238 (1–2): 221–226, Bibcode:1990A&A...238..221B.

[AAA387_1_L285-13] Laureijs, R. J.; et al. (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. （原始内容存档 (PDF)于2017-08-09）.

[BAAS10_630-14] Hershey, J. L.; Borgman, E. R. . Bulletin of the American Astronomical Society. 1978, 10: 630. Bibcode:1978BAAS...10..630H.

[Marcy_&_Benitz-15] Marcy, Geoffrey W.; Benitz, Karsten J. . Astrophysical Journal, Part 1. 1989, 344 (1): 441–453. Bibcode:1989ApJ...344..441M. doi:10.1086/167812.

[kopparapu-2013-16] 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. . 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.

[18] Heinze, A. N.; et al. . 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.

[aaa555_A104-19] Cantrell, Justin R.; et al, , 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.

[Nasa2019-03-07-20] Bill Steigerwald. . NASA. 2019-03-07 [2020-05-12]. （原始内容存档于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.