共生變星 水瓶座 R 星

探索宇宙¹！逐工會揀一幅無仝款 ê 影像抑是相片，𤆬你熟似咱這个迷人 ê 宇宙，閣有專業天文學者²為你解說³。

• 原始文章：Symbiotic R Aquarii
• 影像來源：X-光：NASA/CXC/SAO/R. Montez et al.; 光學：資料來源：NASA/ESA/STScI, 資料處理：Judy Schmidt (CC BY-NC-SA)
• 台文翻譯：An-Li Tsai (NCU)

[漢羅] 共生變星 水瓶座 R 星

變星 水瓶座 R 星 實際上是一組雙星系統，這兩粒 看起來是有密切 ê 共生關係。 這張是太空望遠鏡翕 ê 光學 kah X-光 ê 組合影像，中央這粒離咱有 710 光年遠。 這个趣味 ê 系統有一粒較冷 ê 紅巨星 kah 一粒較高溫較實密 ê 白矮星，攏踅 in 共同 ê 質量中心 leh 行。 你若是用雙筒望遠鏡來 kā 看，to̍h 會發現 水瓶座 R 星 tī 一冬左右 ê 時間 沓沓仔改變伊 ê 光度。 這个雙星系統 ê 可見光主要是 ùi 紅巨星來 ê。 這是一粒 Mira-型 ê 長週期 變星。 包 tī 較冷彼粒巨星外口 ê 物質，會去予重力搝到較細粒、較實密彼粒白矮星。 落尾會 引起 熱核爆炸，kā 物質噴到太空中。 天文學家 tī 過去幾若十年捌看過這款爆發。 相片內底紅色 kah 藍色 ê 就是哈伯太空望遠鏡翕著 ê。 這款美麗 ê 結構 差不多有 1 光年闊，這是一个較老 ê 爆發 ê 觀測證據。 這个觀測資料是 ùi Chandra X-光 天文台（茄仔色）來 ê。 內底是白矮星 ê 噴流 kah 伊邊仔 ê 物質相挵，產生 ê X-光 衝擊波。

[POJ] Kiōng-seng Piàn-seng Chúi-pân-chō R chhiⁿ

Piàn-seng Chúi-pân-chō R chhiⁿ si̍t-chè-siōng sī chi̍t-cho͘ siang-chhiⁿ-hē-thóng, chi̍t nn̄g-lia̍p khòaⁿ--khí-lâi sī ū bi̍t-chhiat ê kiōng-seng koan-hē. Chit-tiuⁿ sī thài-khong bōng-oán-kiàⁿ hip ê kng-ha̍k kah X-kng ê cho͘-ha̍p iáⁿ-siōng, tiong-ng chit-lia̍p lī lán ū chhit-pah-it kng-nî hn̄g. Chit-ê chhù-bī ê hē-thóng ū chi̍t-lia̍p khah léng ê âng-kū-chhiⁿ kah chi̍t-lia̍p khah ko-un khah cha̍t-ba̍t ê pe̍h-é-chhiⁿ, lóng se̍h in kiōng-tông ê chit-liōng-tiong-sim leh kiâⁿ. Lí nā-sī iōng siang-tâng bōng-oán-kiàⁿ lâi kā khòaⁿ, to̍h ē hoat-hiān Chúi-pân-chō R chhiⁿ tī chi̍t tang chó-iū ê sî-kan tau̍h-tau̍h-á kái-piàn i ê kng-tō͘. Chit-ê siang-chhiⁿ hē-thóng ê khó-kiàn-kng chú-iàu sī ùi âng-kū-chhiⁿ lâi ê. Che sī chi̍t-lia̍p Mira-hêng ê tn̂g-chiu-kî piàn-seng. Pau tī khah léng hit-lia̍p kū-chhiⁿ gōa-kháu ê bu̍t-chit, ē khì hō͘ tiōng-le̍k giú kàu khah sè-lia̍p, khah cha̍t-ba̍t hit-lia̍p pe̍h-é-chhiⁿ. Lo̍h-bóe ē ín-khí jia̍t-he̍k-po̍k-chà, kā bu̍t-chit phùn kàu thài-khong tiong. Thian-bûn-ha̍k-ka tī kòe-khì kúi-ā cha̍p nî bat khòaⁿ-kòe chit-khoán po̍k-hoat. Siòng-phìⁿ lāi-té âng-sek kah nâ-sek ê tō-sī Ha-peh-thài-khong-bōng-oán-kiàⁿ hip-tio̍h ê. Chit-khoán bí-lē ê kiat-kò͘ chha-put-to ū chi̍t kng-nî khoah, che sī chi̍t-ê khah lāu ê po̍k-hoat ê koan-chhek chèng-kù. Chit-ê koan-chhek chu-liāu sī ùi Chandra X-kng Thian-bûn-tâi (kiô-á-sek) lâi ê. Lāi-té sī pe̍h-é-chhiⁿ ê phùn-liû kah i piⁿ-á ê bu̍t-chit sio-lòng, sán-seng ê X-kng chhiong-kek-phō.

[KIP] Kiōng-sing Piàn-sing Tsuí-pân-tsō R tshinn

Piàn-sing Tsuí-pân-tsō R tshinn si̍t-tsè-siōng sī tsi̍t-tsoo siang-tshinn-hē-thóng, tsi̍t nn̄g-lia̍p khuànn--khí-lâi sī ū bi̍t-tshiat ê kiōng-sing kuan-hē. Tsit-tiunn sī thài-khong bōng-uán-kiànn hip ê kng-ha̍k kah X-kng ê tsoo-ha̍p iánn-siōng, tiong-ng tsit-lia̍p lī lán ū tshit-pah-it kng-nî hn̄g. Tsit-ê tshù-bī ê hē-thóng ū tsi̍t-lia̍p khah líng ê âng-kū-tshinn kah tsi̍t-lia̍p khah ko-un khah tsa̍t-ba̍t ê pe̍h-é-tshinn, lóng se̍h in kiōng-tông ê tsit-liōng-tiong-sim leh kiânn. Lí nā-sī iōng siang-tâng bōng-uán-kiànn lâi kā khuànn, to̍h ē huat-hiān Tsuí-pân-tsō R tshinn tī tsi̍t tang tsó-iū ê sî-kan ta̍uh-ta̍uh-á kái-piàn i ê kng-tōo. Tsit-ê siang-tshinn hē-thóng ê khó-kiàn-kng tsú-iàu sī uì âng-kū-tshinn lâi ê. Tse sī tsi̍t-lia̍p Mira-hîng ê tn̂g-tsiu-kî piàn-sing. Pau tī khah líng hit-lia̍p kū-tshinn guā-kháu ê bu̍t-tsit, ē khì hōo tiōng-li̍k giú kàu khah sè-lia̍p, khah tsa̍t-ba̍t hit-lia̍p pe̍h-é-tshinn. Lo̍h-bué ē ín-khí jia̍t-hi̍k-po̍k-tsà, kā bu̍t-tsit phùn kàu thài-khong tiong. Thian-bûn-ha̍k-ka tī kuè-khì kuí-ā tsa̍p nî bat khuànn-kuè tsit-khuán po̍k-huat. Siòng-phìnn lāi-té âng-sik kah nâ-sik ê tō-sī Ha-peh-thài-khong-bōng-uán-kiànn hip-tio̍h ê. Tsit-khuán bí-lē ê kiat-kòo tsha-put-to ū tsi̍t kng-nî khuah, tse sī tsi̍t-ê khah lāu ê po̍k-huat ê kuan-tshik tsìng-kù. Tsit-ê kuan-tshik tsu-liāu sī uì Chandra X-kng Thian-bûn-tâi (kiô-á-sik) lâi ê. Lāi-té sī pe̍h-é-tshinn ê phùn-liû kah i pinn-á ê bu̍t-tsit sio-lòng, sán-sing ê X-kng tshiong-kik-phō.

[English] Symbiotic R Aquarii

Variable star R Aquarii is actually an interacting binary star system, two stars that seem to have a close symbiotic relationship. Centered in this space-based optical/x-ray composite image it lies about 710 light years away. The intriguing system consists of a cool red giant star and hot, dense white dwarf star in mutual orbit around their common center of mass. With binoculars you can watch as R Aquarii steadily changes its brightness over the course of a year or so. The binary system's visible light is dominated by the red giant, itself a Mira-type long period variable star. But material in the cool giant star's extended envelope is pulled by gravity onto the surface of the smaller, denser white dwarf, eventually triggering a thermonuclear explosion, blasting material into space. Astronomers have seen such outbursts over recent decades. Evidence for much older outbursts is seen in these spectacular structures spanning almost a light-year as observed by the Hubble Space Telescope (in red and blue). Data from the Chandra X-ray Observatory (in purple) shows the X-ray glow from shock waves created as a jet from the white dwarf strikes surrounding material.

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