1993年、アークトゥルスとポルックスと共に視線速度の観測が行われた。その結果アルデバランの視線速度の有意な変動が検出された。伴星が存在することによるケプラー運動が視線速度の変動の原因だと解釈した場合、アルデバランAから約 2 au (約3億 km) 離れた距離を643日で公転している、下限質量が木星の11.4倍の惑星か褐色矮星が存在する可能性があるとされた[30]。調査した3つの恒星全てに、何かしらの天体が存在することを示唆する観測結果が得られた。ただしこの観測を報告した研究者らは、惑星か褐色矮星の低質量の天体が存在する可能性を否定はしなかったものの、視線速度の変動は恒星固有の、自転によるものか非動径方向の脈動によって引き起こされている可能性が高いと結論付けた[30]。
これらとは別に、プトレマイオス『アルマゲスト』での記述から、「アイン・アッ=サウル」[注 20] عين الثور ʿayn aṯ-ṯawr / ʿayn al-thawr (“牡牛の目”)とも呼ばれた[46]。
これと似たもので、「カルブ・アッ=サウル」[注 21] قلب الثور qalb aṯ-ṯawr / qalb al-thawr (“牡牛の心臓”)という名もあった[47]。ただし、これは本当の名前ではなく、「カルブ・アル=アサド」[注 22] قلب الأسد qalb al-asad (“ライオンの心臓”、レグルス)や「カルブ・アル=アクラブ」[注 23] قلب العقرب qalb al-ʿaqrab (“さそりの心臓”、アンタレス)と混同したものらしい[48]。
^発音は「アルダバラーン」ではなく 「アッダバラーン」 /Ɂaddabaˈra:n/ (太字下線部分にアクセント)。アラビア語の定冠詞「アル」اﻟ al は、後ろに t,d; s,z; r; n などの子音で始まる語が続くと、それと同化して「アッ~」 at-t...,ad-d...; as-s...,az-z...; ar-r...; 「アン~」an-n... などと発音される。
^アラビアの古い星名は、長い間、口承で伝えられて来て、書物に記録されるようになった頃には、アラブの人たちにも本来の意味が分からなくなっていた。そのため、民間語源的なさまざまな解釈が試みられた。「アッ=ダバラーン」の解釈についても、その可能性がある。Kunitzsch (1961), pp. 20–21.
^「〔牡牛の〕南の目にある、赤みがかった、ヒュアデスの明るい〔星〕」(ὁ λαμπρὸς τῶν Ὑάδων ἐπὶ τοῦ νοτίου ὀφθαλμοῦ ὑπόκιρρος)となっている。Kunitzsch (1959), p. 109; J. L. Heiberg (ed.), Claudii Ptolemaei opera quae extant omnia, Vol. I: Syntax mathematica, Leipzig: Teubner 1898-1903, Pars II, p.88; プトレマイオス(藪内清訳)『アルマゲスト』〔フランス語訳からの重訳〕、恒星社厚生閣、新版1982年 (初版1949, 58年)、334頁。
^「ヒュアデスの明るくて赤みがかった〔星〕で、また『ランパディアース』 と呼ばれる〔星〕」(ὁ μὲν λαμπρὸς τῆς Ὑάδος καὶ ὑπόκιρρος, καλούμενος δὲ Λαμπαδίας) とある。Ptolemy, Tetrabiblos, ed. & tr. by F. E. Robbins (The Loeb Classical Library), Norwich, 1940, p.46.
^F. Gaffiot, Diccionaire Latin Français, Paris: Hachette, 1934 の Pălīlĭcĭum sīdus の項には、「ヒュアデスの1つ〔の星〕」une des Hyades とある。
^コペルニクスは『天球回転論』第2巻の恒星表で、おうし座第14星について、「目そのものにあって輝いている、ローマ人たちがパリーリキウムと呼んだ〔星〕」 (In ipso oculo luce[n]s paliliciu[m] dicta Ro[manis])と言っている。N. Copernicus, De revolutionibus orbium coelestium, Nürnberg, 1543, fol.52v; コペルニクス(高橋憲一 訳・解説)『天球回転論』 みすず書房、2017年、128頁。なお、この訳では (おそらくLewis and Short, A Latin Dictionary の見出し Palīlīcius に従って)「パリーリーキウス」 としているが、「パリーリキウム」とするのが適切である。
^これらの別名は、古い名前である「アッ=ダバラーン」が “プレイアデスの後を追うもの”と解釈された後に生まれた可能性がある。Kunitzsch (1959), p. 109.
^2語に切らないで続けて読むときは「ターリユンナジュム」tāliyu n-naǧm (/ˈta:lijunˈnaʤm/) と発音する。前の語に主格語尾 –u が付き、定冠詞 al- の a が脱落する。
^「ナジュム」は一般的には “星” という意味だが、ここではプレイアデスを指す。なお、プレイアデスに固有の名前は「アッ=スライヤー」 الثريّا aṯ-ṯurayyā / al-thurayyā で、これはアラビアで古くから広く知られた星名の1つである。Kunitzsch (1961), pp. 114-115 (Nr. 306); pp. 20-21.
^ビールーニー(10-11世紀)が『過去の足跡』で次のように言っている。「〔ダバラーンは〕また、ファニークとも呼ばれる。〔ファニークとは〕大きなラクダである。〔そう呼ばれるのは〕、その周りの星々を〔アラブの人たちは〕キラースと呼んでいるからである。」ويسمّى أيضًا الفنيق وهو الجمل العظيم لأنّهم يسمّون الكواكب التي حوله القلاص . al-Bīrūnī, Al-Āṯār al-bāqiya ʿan al-qarūn al-ḫāliya, ed. C. E. Sachau, Leipzig, 1878, p. 342.
^ abPaul Kunitzsch; Tim Smart (2006). A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations. Sky Publishing. p. 54. ISBN978-1-931559-44-7
^ abRichichi, A.; Roccatagliata, V. (2005). “Aldebaran's angular diameter: How well do we know it?”. Astronomy & Astrophysics433 (1): 305–312. arXiv:astro-ph/0502181. Bibcode: 2005A&A...433..305R. doi:10.1051/0004-6361:20041765. "We derive an average value of 19.96±0.03 milliarcsec for the uniform disk diameter. The corresponding limb-darkened value is 20.58±0.03 milliarcsec, or 44.2±0.9 R☉."
^Koncewicz, R.; Jordan, C. (January 2007). “OI line emission in cool stars: calculations using partial redistribution”. Monthly Notices of the Royal Astronomical Society374 (1): 220–231. Bibcode: 2007MNRAS.374..220K. doi:10.1111/j.1365-2966.2006.11130.x.
^ abcA. P. Hatzes; et al. (13 May 2015). "Long-lived, long-period radial velocity variations in Aldebaran: A planetary companion and stellar activity". arXiv:1505.03454v1 [astro-ph.EP]。
^Lynn, W. T. (1885). “Occultation of Aldebaran in the sixth century. - Bliss, Astronomer Royal”. The Observatory8: 86. Bibcode: 1885Obs.....8...86L.
^Halley, Edmund (1717). “Considerations on the Change of the Latitudes of Some of the Principal Fixt Stars. By Edmund Halley, R. S. Sec”. Philosophical Transactions (1683-1775)30: 736. Bibcode: 1717RSPT...30..736H. doi:10.1098/rstl.1717.0025.
^Pease, F. G. (June 1921). “The Angular Diameter of a Bootis by the Interferometer”. Publications of the Astronomical Society of the Pacific33 (193): 171. Bibcode: 1921PASP...33..171P. doi:10.1086/123068.
^Richichi & Roccatagliata (2005) derived an angular diameter of 20.58±0.03 milliarcsec, which given a distance of 65 light years yields a diameter of 61 million km.
^Cutri, R. M.; Skrutskie, M. F.; Van Dyk, S.; Beichman, C. A.; Carpenter, J. M.; Chester, T.; Cambresy, L.; Evans, T. et al. (2003). “VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)”. VizieR On-line Data Catalog: II/246. Originally published in: 2003yCat.2246....0C2246. Bibcode: 2003yCat.2246....0C.
^Können, G. P.; Meeus, J. (1972). “Occultation series of five stars”. Journal of the British Astronomical Association82: 431. Bibcode: 1972JBAA...82..431K.
^Poveda, A. et al. (April 1994). “Statistical studies of visual double and multiple stars. II. A catalogue of nearby wide binary and multiple systems”. Revista Mexicana de Astronomia y Astrofisica28 (1): 43–89. Bibcode: 1994RMxAA..28...43P.
Kunitzsch, Paul (1959). Arabische Sternnamen in Europa. Wiesbaden: Otto Harrassowitz
Kunitzsch, Paul (1961). Untersuchungen zur Sternnomenklatur der Araber. Wiesbaden: Otto Harrassowitz
Kunitzsch, Paul (1983). Über eine anwāʾ-Tradition mit bisher unbekannten Sternnamen (= Sitzungsberichte der Bayerischen Akademie der Wissenschaften, Philosophisch-Historische Klasse', Jahrgang 1983, Heft 5). München: Beck
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