米拉
维基百科,自由的百科全书
觀測資料 曆元 J2000.0 |
|
---|---|
星座 | 鯨魚座 |
赤經 | 02h 19m 20.79s |
赤緯 | -02° 58′ 39.5″ |
視星等 (V) | 2.0 to 10.1 |
特性 | |
光譜分類 | M7IIIe |
B-V 色指數 | 1.42 |
U-B 色指數 | 1.09 |
變星類型 | 米拉變星 |
天體測定 | |
視向速度 (Rv) | +63.8 km/s |
固有運動 (μ) | RA: 10.33 mas/yr Dec.: -239.48 mas/yr |
視差 (π) | 7.79 ± 1.07 mas |
距離 | {{{dist_ly}}} ly ({{{dist_pc}}} pc) |
絕對星等 (MV) | 0.93 |
詳情 | |
質量 | 1.2 M☉ |
半徑 | 500 R☉ |
光度 | 15,000 L☉ |
溫度 | 2,200 K |
金屬度 | ? |
自轉 | ? |
年齡 | ? 年 |
其他命名 | |
68 Ceti
|
米拉 (中名蒭藁增二,鯨魚座ο)是一顆紅巨星,位於鯨魚座,距離地球約418光年。米拉是一對聯星,主星米拉A是巨星,半星米拉B是白矮星。米拉A本身是一顆振盪的變星,可能是除了大凌五之外,第一顆被發現的非超新星變星。而除了怪異的船底座η之外,米拉是天空中最明亮的週期變星,但在週期內部分的時間會成為肉眼看不見的10等星。他的距離並不是很正確的,在希巴谷衛星探測之前被認為是約220光年,之後的資料認為是417光年,但是誤差可能高達14%。
伴星是在1995年由哈柏太空望遠鏡拍攝的影像中解析出來的,在1997年推導出伴星與主星相距70AU。哈柏的紫外線影像和後來錢卓望遠鏡的X射線影像顯示有一道螺旋的氣流離開米拉A朝向米拉B而去。伴星圍繞米拉的軌道週期約為400年。
Mira became the "type" star of the long-period "Mira variables". It — and the other 6000 or so known stars of this class — are all red giants whose surfaces oscillate in such a way as to increase and decrease in brightness over periods ranging from about 80 days to more than 1000. In the particular case of Mira, its increases in brightness take it up to about magnitude 3.5 on average, which is a fairly noticeable star. Individual cycles vary too; well-attested maxima go as high as magnitude 2.0 in brightness and as low as 4.9, a range almost 15 times in brightness, and there are historical suggestions that the real spread may be three times this or more. Minima range much less, and have historically been between 8.6 and 10.1, a factor of four times in luminosity. The total swing in brightness from absolute maximum to absolute minimum (two events which did not occur on the same cycle) is 1700 times. Interestingly, since Mira emits the vast majority of its radiation in the infrared, its variability in that band is only about two magnitudes.(2) The shape of its light curve is of an increase over about 100 days, and a return twice as long. A recent lightcurve is available from the BAV ([1]).
目录 |
[编辑] Discovery
Mira was discovered (or at least noted as special for the first time) after a series of observations by the astronomer David Fabricius beginning on August 3, 1596. Observing the planet Mercury, he needed a reference star for comparing positions and picked a previously unremarked third-magnitude star nearby. By August 21, however, it had increased in brightness by one magnitude, then by October had faded from view. Fabricius assumed it was a nova — interesting enough — but then saw it again on February 16, 1609.
Eventually, Johann Holwarda determined a period of the star's reappearances, eleven months; Johannes Hevelius was observing it at the same time and named it "Mira" (meaning "Wonderful") in 1662's Historiola Mirae Stellae, for it acted like no other known star in the sky. Ismail Bouillaud then nailed the period down to 333 days, less than one day off of the modern value of 332 days (and perfectly forgivable, as Mira is known to vary slightly in period, and may even be slowly changing over time).
There is considerable speculation as to whether or not Mira had been observed prior to Fabricius. Certainly Algol's history (known for certain as a variable only in 1667, but with legends and such stretching back to antiquity showing that it had been observed with suspicion for millennia) suggested that Mira might have been known too. Karl Manitius, a translator of Hipparchus' Commentary on Aratus, has suggested that certain lines from that second century BC text may be about Mira. The other usual pre-telescopic Western suspects -- the catalogs of Ptolemy, al-Sufi, Ulugh Beg, and Tycho Brahe -- turn up no mentions, even as a regular star. There are three observations from Chinese and Korean archives, in 1596, 1070, and the same year when Hipparchus would have made his observation (134 BC) that are suggestive, but the Chinese practice of pinning down observations no more precisely than within a given Chinese constellation makes it difficult to be sure.
[编辑] 參考資料
- Robert Burnham Jr.,Burnham's Celestial Handbook, Vol. 1, (New York: Dover Publications, Inc., 1978), 634.
- James Kaler, The Hundred Greatest Stars, (New York: Copernicus Books, 2002), 121.
[编辑] 相關條目
[编辑] 外部鏈結
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[编辑] 資料來源
或許寫這段文章的人的名字也叫做米拉(Mira)