Epsilon Indi
Epsilon Indi
Location of ε Indi (circled)
Observation dataEpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationIndus
Right ascension22h 03m 21.65363s[1]
Declination−56° 47′ 09.5228″[1]
Apparent magnitude (V)4.674±0.006[2]
Characteristics
Spectral typeK5V + T1 + T6[3]
U−B color index1.00[4]
B−V color index1.056±0.016[5]
Astrometry
ε Ind A
Radial velocity (Rv)−40.43±0.13[1] km/s
Proper motion (μ)RA: 3,966.661(86)mas/yr[1]Dec.: −2,536.192(92)mas/yr[1]
Parallax (π)274.8431±0.0956 mas[1]
Distance11.867 ± 0.004 ly (3.638 ± 0.001 pc)
Absolute magnitude (MV)6.89[6]
ε Ind Ba/Bb
Parallax (π)270.6580±0.6896 mas[7]
Distance12.05 ± 0.03 ly (3.695 ± 0.009 pc)
Orbit[8]
Primaryε Ind Ba
Companionε Ind Bb
Period (P)11.0197 ± 0.0076 yr
Semi-major axis (a)661.58 ± 0.37 mas(2.4058 ± 0.0040 au)
Eccentricity (e)0.54042 ± 0.00063
Inclination (i)77.082 ± 0.032°
Longitude of the node (Ω)147.959 ± 0.023°
Argument of periastron (ω)(secondary)328.27 ± 0.12°
Details
ε Ind A
Mass0.782±0.023[9] M☉
Radius0.713±0.006[9] R☉
Luminosity0.21±0.02[10] L☉
Surface gravity (log g)4.50±0.07[9] cgs
Temperature4,649 ± 65 [ 9 ]  K
金属量[Fe/H]−0.17 ± 0.04 [ 9 ] デックス
回転35.732+0.006 −0.003日数[ 11 ]
回転速度（v  sin  i）2.00 [ 10 ]  km/s
年3.5+0.8 −1.0[ 8 ] ジル
ε インドバ/バ♭
質量バ： 66.92 ± 0.36  MジュピターBb: 53.25 ± 0.29 [ 8 ]  M Jup
半径Ba: 約0.080–0.081  R ☉ Bb: 約0.082–0.083 [ 12 ]  R ☉
明るさバ： 2.04 × 10 −5  L ☉ Bb: 5.97 × 10 −6 [ 8 ]  L ☉
表面重力（log  g）Ba: 5.43–5.45 Bb: 5.27–5.33 [ 12 ]  cgs
温度Ba: 1,352–1,385 K Bb: 976–1,011 [ 12 ]  K
その他の指定
UGP 544、ε Ind、CD −57°8464、CPD −57°10015、FK5 825、GJ 845、HD 209100、HIP 108870、HR 8387、SAO 247287、LHS 67 [ 13 ]
データベース参照
シンバッドシステム
あ
バブ
Bab（X線源として）
太陽系外惑星アーカイブデータ

イプシロン・インディ（ε Indi のラテン語表記）は、南の星座インダス座にあり、地球から約12光年の距離にある恒星系である。この恒星はオレンジ色をしており、見かけの視等級は4.674で、肉眼でかすかに見える。[ 2 ] K型主系列星ε Indi A と、その周りを広い軌道で回る2つの褐色矮星ε Indi Ba および ε Indi Bbで構成される。 [ 14 ]褐色矮星は2003年に発見された。 ε Indi Ba は早期T型矮星（T1）、ε Indi Bb は後期T型矮星（T6）で、主星からの投影距離は1460 AUである。

ε Indi A has one known planet, ε Indi Ab, with a mass of 6.31 Jupiter masses in an elliptical orbit with a period of about 171.3 years. ε Indi Ab is the second-closest Jovian exoplanet, after ε Eridani b. The ε Indi system provides a benchmark case for the study of the formation of gas giants and brown dwarfs.[11]

Observation

Epsilon Indi with SkyMapper and a Hubble NICMOS image of the brown dwarf binary

The constellation Indus (the Indian) first appeared in Johann Bayer's celestial atlas Uranometria in 1603. The 1801 star atlas Uranographia, by German astronomer Johann Elert Bode, places ε Indi as one of the arrows being held in the left hand of the Indian.[15]

In 1847, Heinrich Louis d'Arrest compared the position of this star in several catalogues dating back to 1750, and discovered that it possessed a measureable proper motion. That is, he found that the star had changed position across the celestial sphere over time.[16] In 1882–3, the parallax of ε Indi was measured by astronomers David Gill and William L. Elkin at the Cape of Good Hope. They derived a parallax estimate of 0.22 ± 0.03 arcseconds.[17] In 1923, Harlow Shapley of the Harvard Observatory derived a parallax of 0.45 arcseconds.[18]

In 1972, the Copernicus satellite was used to examine this star for the emission of ultraviolet laser signals. Again, the result was negative.[19] ε Indi leads a list, compiled by Margaret Turnbull and Jill Tarter of the Carnegie Institution in Washington, of 17,129 nearby stars most likely to have planets that could support complex life.[20]

The star is among five nearby paradigms as K-type stars of a type in a 'sweet spot' between Sun-analog stars and M stars for the likelihood of evolved life, per analysis of Giada Arney from NASA's Goddard Space Flight Center.[21]

Characteristics

εインディAは、スペクトル型K5Vの主系列星である。この星の質量は太陽の約4分の3 [ 22 ]であり、半径は太陽の71%である[ 10 ]。表面重力は太陽よりわずかに大きい[ 4 ] 。星の金属度は、ヘリウムよりも原子番号が大きい元素の割合であり、通常は鉄と水素の比で表され、太陽の同じ比率と比較される。εインディAの光球における鉄の割合は、太陽の約87%であることがわかっている[ 3 ]。

εインディAのコロナは太陽に似ており、X線輝度は2 × 1027 エルグ s −1 (2 × 1020  W）と推定されるコロナ温度は2 × 106  K。この恒星の恒星風は外側に広がり、63 AUの距離に弓状衝撃波を形成する。弓状衝撃波の下流では、終端衝撃波が恒星から140 AUまで到達する。 [ 23 ]

インドεから見たおおぐま座の太陽とケンタウルス座α星の位置

この星は、肉眼で見える恒星の中ではグルームブリッジ1830と白鳥座61番星に次いで3番目に大きい固有運動をしており[ 24 ]、全体では9番目に大きい。[ 25 ]この運動により、この星は西暦2640年頃にきょうだい座に移動する。 [ 26 ] ε インディ A の太陽に対する相対的な 空間速度は86 km/sであり[ 4 ] [注 1 ] 、これは若い恒星と考えられているものとしては異常に高い。[ 27 ]この恒星は、少なくとも16個のI族の恒星からなる ε インディ移動グループの一員であると考えられている。[ 28 ]これは、同様の空間速度ベクトルを持つ恒星の集まりであるため、同じ時間と場所で形成された可能性が高い。[ 29 ] εインディは約17,500年後に近日点を通過し、約10.58光年（3.245パーセク）の距離まで太陽に最接近します。 [ 30 ]

As seen from ε Indi, the Sun is a 2.6-magnitude star in Ursa Major, near the bowl of the Big Dipper.[note 2]

Brown dwarfs

Artist's conception of the Epsilon Indi system showing Epsilon Indi A and its brown-dwarf binary companions. The labels give the initial minimum measurement of the distance between Epsilon Indi A and the binary.[31]

In January 2003, astronomers announced the discovery of a brown dwarf with a mass of 40 to 60 Jupiter masses in orbit around ε Indi A with a projected separation on the sky of about 1,500 AU.[32][33] In August 2003, astronomers discovered that this brown dwarf was actually a binary brown dwarf, with an apparent separation of 2.1 AU and an orbital period of about 15 years.[12][34] Both brown dwarfs are of spectral class T; the more massive component, ε Indi Ba, is of spectral type T1–T1.5 and the less massive component, ε Indi Bb, of spectral type T6.[12] More recent parallax measurements with the Gaia spacecraft place the ε Indi B binary about 11,600 AU (0.183 lightyears) away from ε Indi A, along line of sight from Earth.[7]

Evolutionary models[35] have been used to estimate the physical properties of these brown dwarfs from spectroscopic and photometric measurements. These yield masses of 47 ± 10 and 28 ± 7 times the mass of Jupiter, and radii of 0.091 ± 0.005 and 0.096 ± 0.005solar radii, for ε Indi Ba and ε Indi Bb, respectively.[36] The effective temperatures are 1300–1340 K and 880–940 K, while the log g (cm s−1) surface gravities are 5.50 and 5.25, and their luminosities are 1.9 × 10−5 and 4.5 × 10−6 the luminosity of the Sun. They have an estimated metallicity of [M/H] = –0.2.[12]

Planetary system

The Epsilon Indi A planetary system[37]
Companion(in order from star)MassSemimajor axis(AU)Orbital period(years)EccentricityInclinationRadius
b7.29+0.60−0.61 MJ29.2+3.3−3.4180+32−310.399+0.059−0.076105.4+2.5−2.4°1.08[a] RJ
Epsilon Indi Ab imaged by JWSTMIRI. The star marks the position of its host star, whose light is blocked by a coronagraph.

The existence of a planetary companion to Epsilon Indi A was suspected since 2002 based on radial velocity observations.[38] The planet Epsilon Indi Ab was confirmed in 2018[39] and formally published in 2019 along with its detection via astrometry.[11]

A direct imaging attempt of this planet using the James Webb Space Telescope was performed in 2023,[40] and the image was released in 2024. The detected planet's mass and orbit are different from what was predicted based on radial velocity and astrometry observations.[41] It has a mass of 6.31 Jupiter masses and an elliptical orbit with a period of about 171.3 years.[42]

No excess infrared radiation that would indicate a debris disk has been detected around ε Indi.[43] Such a debris disk could be formed from the collisions of planetesimals that survive from the early period of the star's protoplanetary disk.

See also

Notes

  1. ^The space velocity components are: U = −77; V = −38, and W = +4. This yields a net space velocity of 772 + 382 + 42 = 86{\displaystyle {\begin{smallmatrix}{\sqrt {77^{2}\ +\ 38^{2}\ +\ 4^{2}}}\ =\ 86\end{smallmatrix}}} km/s.
  2. ^From ε Indi the Sun would appear on the diametrically opposite side of the sky at the coordinates RA=10h 03m 21s, Dec=56° 47′ 10″, which is located near Beta Ursae Majoris. The absolute magnitude of the Sun is 4.8, so, at a distance of 3.63 parsecs, the Sun would have an apparent magnitude m = Mv + 5⋅((log10⁡ 3.63) − 1) = 2.6{\displaystyle {\begin{smallmatrix}m\ =\ M_{v}\ +\ 5\cdot ((\log _{10}\ 3.63)\ -\ 1)\ =\ 2.6\end{smallmatrix}}}.
  1. ^Calculated, using the Stefan-Boltzmann law and the planet's effective temperature and luminosity, with respect to the being the solar nominal effective temperature of 5,772 K:(5,772275)4⋅10−7.2=0.1106 R⊙.{\displaystyle {\sqrt {{\biggl (}{\frac {5,772}{275}}{\biggr )}^{4}\cdot 10^{-7.2}}}=0.1106\ R_{\odot }.}

References

  1. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). 「Gaiaデータリリース3. コンテンツとサーベイプロパティの概要」 .天文学と天体物理学. 674 : A1. arXiv : 2208.00211 . Bibcode : 2023A&A...674A...1G . doi : 10.1051/0004-6361/202243940 . S2CID  244398875 .VizieRにおけるこのソースの Gaia DR3 レコード。
  2. ^ a b Paunzen, E. (2015-08-01). 「Strömgren-Crawford uvbyβ測光法の新しいカタログ」.天文学と天体物理学. 580 : A23. arXiv : 1506.04568 . Bibcode : 2015A&A...580A..23P . doi : 10.1051/0004-6361/201526413 . ISSN 0004-6361 . 
  3. ^ a b Demory, Brice-Olivier;セグランサン、ダミアン。フォルヴェイユ、ティエリー。ケロス、ディディエ。ブジット、ジャン＝リュック。 Delfosse, Xavier;ディ・フォルコ、エマニュエル。ケルベラ、ピエール。ル・ブーカン、ジャン＝バティスト。ペリエ、クリスチャン。ベニスティ、ミリアム。デュベール、ジル。ホフマン、カール・ハインツ。ロペス、ブルーノ。 Petrov, Romain (October 2009). 「VLTI で再検討された低質量星の質量と超低質量星の質量半径関係」。天文学と天体物理学。505 (1): 205– 215. arXiv : 0906.0602 . Bibcode : 2009A&A...505..205D . doi : 10.1051/0004-6361/200911976 . S2CID 14786643 . 
  4. ^ a b c Kollat​​schny, W. (1980). 「後期型矮星イプシロン・インディのモデル大気」.天文学と天体物理学. 86 (3): 308– 314.書誌コード: 1980A&A....86..308K .
  5. ^ van Leeuwen, F. (2007). 「新しいヒッパルコス還元の検証」.天文学と天体物理学. 474 (2): 653– 664. arXiv : 0708.1752 . Bibcode : 2007A&A...474..653V . doi : 10.1051/0004-6361:20078357 . S2CID 18759600 . 
  6. ^Jimenez, Raul; Flynn, Chris; MacDonald, James; Gibson, Brad K. (March 2003). "The Cosmic Production of Helium". Science. 299 (5612): 1552–1555. arXiv:astro-ph/0303179. Bibcode:2003Sci...299.1552J. doi:10.1126/science.1080866. PMID 12624260. S2CID 1424666.
  7. ^ abVallenari, 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.
  8. ^ abcdChen, Minghan; Li, Yiting; Brandt, Timothy D.; Dupuy, Trent J.; Cardoso, Cátia V.; McCaughrean, Mark J. (2022). "Precise Dynamical Masses of ε Indi Ba and Bb: Evidence of Slowed Cooling at the L/T Transition". The Astronomical Journal. 163 (6): 288. arXiv:2205.08077. Bibcode:2022AJ....163..288C. doi:10.3847/1538-3881/ac66d2. S2CID 248834536.
  9. ^ abcdeLundkvist, Mia S.; Kjeldsen, Hans; Bedding, Timothy R.; McCaughrean, Mark J.; Butler, R. Paul; Slumstrup, Ditte; Campante, Tiago L.; Aerts, Conny; Arentoft, Torben; Bruntt, Hans; Cardoso, Cátia V.; Carrier, Fabien; Close, Laird M.; da Silva, João Gomes; Kallinger, Thomas; King, Robert R.; Li 李, Yaguang 亚光; Murphy, Simon J.; Rørsted, Jakob L.; Stello, Dennis (2024-04-01). "Low-amplitude Solar-like Oscillations in the K5 V Star ϵ Indi A". The Astrophysical Journal. 964 (2): 110. arXiv:2403.04509. Bibcode:2024ApJ...964..110L. doi:10.3847/1538-4357/ad25f2. ISSN 0004-637X.
  10. ^ a b c Rains, Adam D.; et al. (2020年4月). 「VLTI/PIONIERによる南半球16星の精密角直径」 . Monthly Notices of the Royal Astronomical Society . 493 (2): 2377– 2394. arXiv : 2004.02343 . Bibcode : 2020MNRAS.493.2377R . doi : 10.1093/mnras/staa282 .
  11. ^ a b c Feng, Fabo;アングラダ・エスクデ、ギエム。 Tuomi, Mikko;ジョーンズ、ヒュー・RA。シャナメ、フリオ。 Butler, Paul R.; Janson, Markus (14 October 2019). 「動径速度と天文データにおける最も近い木星の類似体の検出」。王立天文協会の月次通知。490 (4): 5002– 5016. arXiv : 1910.06804 . Bibcode : 2019MNRAS.490.5002F . doi : 10.1093/mnras/stz2912 . S2CID 204575783 . 
  12. ^ a b c d e f King, RR; et al. (2010年2月). 「ɛ Indi Ba, Bb: 最も近い既知の褐色矮星の詳細な研究」(PDF) . Astronomy and Astrophysics . 510 : A99. arXiv : 0911.3143 . Bibcode : 2010A&A...510A..99K . doi : 10.1051/0004-6361/200912981 . S2CID 53550866.しかし、実効温度、表面重力、および光度の推定値が存在する場合でも、低温褐色矮星の質量の導出は不確実であるように思われる。 
  13. ^ "SIMBAD クエリ結果: LHS 67 -- 高い固有運動をもつ星" . Centre de Données astronomiques de Strasbourg . Retrieved 2007-07-11 .
  14. ^ Smith, Verne V.; Tsuji, Takashi; Hinkle, Kenneth H.; Cunha, Katia; Blum, Robert D.; Valenti, Jeff A.; Ridgway, Stephen T.; Joyce, Richard R.; Bernath, Peter (2003). 「褐色矮星 ε Indi Ba の高解像度赤外分光法」. The Astrophysical Journal Letters . 599 (2): L107– L110. arXiv : astro-ph/0311237 . Bibcode : 2003ApJ...599L.107S . doi : 10.1086/381248 . S2CID 117133193 . 
  15. ^"Discovery of Nearest Known Brown Dwarf" (Press release). European Southern Observatory. 2003-01-13. Retrieved 2025-06-14.
  16. ^D'Arrest, M. (1847). "On proper motion of ε Indi". Monthly Notices of the Royal Astronomical Society. 8: 16. Bibcode:1847MNRAS...8...16D. doi:10.1093/mnras/8.1.16.
  17. ^Callandreau, O. (1886). "Revue des publications astronomiques. Heliometer determinations of Stellar parallax, in the southern hemisphere, by David Gill and W. L. Elkin". Bulletin Astronomique (in French). 2 (1): 42–44. Bibcode:1885BuAsI...2...42C.
  18. ^Shapley, Harlow (1923). "Epsilon Indi". Harvard College Observatory Bulletin. 789 (789): 2. Bibcode:1923BHarO.789Q...2S.
  19. ^Lawton, A. T. (1975). "CETI from Copernicus". Spaceflight. 17: 328–330. Bibcode:1975SpFl...17..328L.
  20. ^Stahl, Jason (January 2007). "20 Things You Didn't Know About... Aliens". Discover. Archived from the original on 2007-02-21. Retrieved 2007-03-02.
  21. ^Bill Steigerwald (22 February 2019). ""Goldilocks" Stars May be "Just Right" for Finding Habitable Worlds". NASA. '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.
  22. ^"The 100 nearest star systems". Research Consortium On Nearby Stars. Georgia State University. January 1, 2012. Retrieved 2012-06-11.
  23. ^Müller, Hans-Reinhard; Zank, Gary P. (2001). "Modeling the Interstellar Medium-Stellar Wind Interactions of λ Andromedae and ε Indi". The Astrophysical Journal. 551 (1): 495–506. Bibcode:2001ApJ...551..495M. doi:10.1086/320070.
  24. ^Weaver, Harold F. (1947). "The Visibility of Stars Without Optical Aid". Publications of the Astronomical Society of the Pacific. 59 (350): 232–243. Bibcode:1947PASP...59..232W. doi:10.1086/125956.
  25. ^Staff (2007-05-04). "High Proper Motion Stars: Interesting Areas to View". ESA. Retrieved 2006-08-10.
  26. ^Moore, Patrick; Rees, Robin (2014). Patrick Moore's Data Book of Astronomy. Cambridge: Cambridge University Press. p. 296. ISBN 978-1-139-49522-6.
  27. ^Rocha-Pinto, Helio J.; Maciel, Walter J.; Castilho, Bruno V. (2001). "Chromospherically Young, Kinematically Old Stars". Astronomy and Astrophysics. 384 (3): 912–924. arXiv:astro-ph/0112452. Bibcode:2002A&A...384..912R. doi:10.1051/0004-6361:20011815. S2CID 16982360.
  28. ^Eggen, O. J. (1971). "The zeta Herculis, sigma Puppis, ε Indi, and eta Cephei Groups of Old Disk Population Stars". Publications of the Astronomical Society of the Pacific. 83 (493): 251–270. Bibcode:1971PASP...83..251E. doi:10.1086/129119.
  29. ^Kollatschny, W. (1980). "A model atmosphere of the late type dwarf Epsilon INDI". Astronomy and Astrophysics. 86 (3): 308–314. Bibcode:1980A&A....86..308K.
  30. ^Bailer-Jones, C. A. L. (March 2015). "Close encounters of the stellar kind". Astronomy & Astrophysics. 575: 13. arXiv:1412.3648. Bibcode:2015A&A...575A..35B. doi:10.1051/0004-6361/201425221. S2CID 59039482. A35.
  31. ^"Gemini Detects Something "Cool" in Our Neighborhood: Closest Known Brown Dwarf has a Companion" (Press release). NOIRLab. 2004-10-27. Retrieved 2025-06-13.
  32. ^Scholz, Ralf-Dieter; McCaughrean, Mark (2003-01-13). "Discovery of Nearest Known Brown Dwarf: Bright Southern Star Epsilon Indi Has Cool, Substellar Companion". European Southern Observatory. Archived from the original on October 14, 2007. Retrieved 2006-05-24.
  33. ^Scholz, R.-D.; McCaughrean, M. J.; Lodieu, N.; Kuhlbrodt, B. (February 2003). "ε Indi B: A new benchmark T dwarf". Astronomy and Astrophysics. 398 (3): L29–L33. arXiv:astro-ph/0212487. Bibcode:2003A&A...398L..29S. doi:10.1051/0004-6361:20021847. S2CID 119474823.
  34. ^Volk, K.; Blum, R.; Walker, G.; Puxley, P. (2003). "epsilon Indi B". IAU Circular (8188). IAU: 2. Bibcode:2003IAUC.8188....2V.
  35. ^E.g., Baraffe, I.; Chabrier, G.; Barman, T.; Allard, F.; Hauschildt, P. H. (May 2003). "Evolutionary models for cool brown dwarfs and extrasolar giant planets. The case of HD 209458". Astronomy and Astrophysics. 402 (2): 701–712. arXiv:astro-ph/0302293. Bibcode:2003A&A...402..701B. doi:10.1051/0004-6361:20030252. S2CID 15838318.
  36. ^McCaughrean, M. J.; et al. (January 2004). "ε Indi Ba, Bb: The nearest binary brown dwarf". Astronomy and Astrophysics. 413 (3): 1029–1036. arXiv:astro-ph/0309256. Bibcode:2004A&A...413.1029M. doi:10.1051/0004-6361:20034292. S2CID 15407249.
  37. ^Feng, Fabo; Xiao, Guang-Yao; Jones, Hugh R A; Jenkins, James S; Pena, Pablo; Sun, Qinghui (2024-12-19). "Lessons learned from the detection of wide companions by radial velocity and astrometry". Monthly Notices of the Royal Astronomical Society. 539 (4): 3180–3200. arXiv:2412.14542. doi:10.1093/mnras/staf689. ISSN 0035-8711.
  38. ^Endl, M.; Kürster, M.; Els, S.; Hatzes, A. P.; Cochran, W. D.; Dennerl, K.; Döbereiner, S. (2002). "The planet search program at the ESO Coudé Echelle spectrometer. III. The complete Long Camera survey results". Astronomy and Astrophysics. 392 (2): 671–690. arXiv:astro-ph/0207512. Bibcode:2002A&A...392..671E. doi:10.1051/0004-6361:20020937. S2CID 17393347.
  39. ^Feng, Fabo; Tuomi, Mikko; Jones, Hugh R. A. (23 March 2018). "Detection of the closest Jovian exoplanet in the Epsilon Indi triple system". arXiv:1803.08163 [astro-ph.EP].
  40. ^"A direct detection of the closest Jupiter analog with JWST/MIRI". stsci.edu. STScI. Retrieved 31 July 2022. We will collect the first direct images of a radial velocity planet, by targeting Eps Indi Ab with JWST/MIRI. [...] Our simulations confirm that we will detect Eps Indi Ab's thermal emission at high confidence, regardless of its cloud properties or thermal evolution.
  41. ^"NASA's Webb Images Cold Exoplanet 12 Light-Years Away". nasa.gov. NASA Webb Mission Team. 24 July 2024. Retrieved Jul 24, 2024.
  42. ^Matthews, E. C.; Carter, A. L.; et al. (July 2024). "A temperate super-Jupiter imaged with JWST in the mid-infrared". Nature. 633 (8031): 789–792. arXiv:2503.01599. Bibcode:2024Natur.633..789M. doi:10.1038/s41586-024-07837-8. PMC 11424479. PMID 39048015.
  43. ^Trilling, D. E.; et al. (February 2008). "Debris Disks around Sun-like Stars". The Astrophysical Journal. 674 (2): 1086–1105. arXiv:0710.5498. Bibcode:2008ApJ...674.1086T. doi:10.1086/525514. S2CID 54940779.

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