白矮星 蛇夫座 RS 爆炸

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³解說⁴。

• 原始文章：Explosions from White Dwarf Star RS Oph
• 影像來源 kah 版權：David A. Hardy & PPARC
• 台文翻譯：An-Li Tsai (NCU)

[漢羅] 白矮星 蛇夫座 RS 爆炸

蛇夫座 RS ê 雙星系統到今猶繼續產生壯麗 ê 爆炸現象。 差不多 20 年一改，雙星內底 ê 紅巨星 to̍h 會倒夠額 ê 水素 氣體到伊 ê 星伴 白矮星，予伊 ê 表面產生一改燦爛 ê 熱核爆炸。 In 差不多有 5000 光年 遠。 In 產生 ê 新星 爆炸予 蛇夫座 RS 雙星系統變光到幾若倍，用目睭 to̍h 看有。 紅巨星 to̍h tī 這幅圖 ê 正爿 頂懸，白矮星 to̍h tī 倒爿彼个足光 ê 吸積盤 ê 中央。 雙星 互相踅對方 leh 行 ê 時陣，氣體 to̍h ùi 紅巨星 走去 白矮星。 天文學家 推算，閣 10 萬年了後，這个雙星系統會 tī 白矮星 累積夠額 ê 物質。 等超過 Chandrasekhar 極限 了後，to̍h 會產生能量閣較強、上尾一改 ê 超新星 爆炸。 Ùi 這個月頭開始，你 to̍h 會當看著 蛇夫座 RS 閣變做 足光 ê 新星 爆炸 矣。

[POJ] Pe̍h-é-chhiⁿ Siâ-hu-chō RS po̍k-chà

Siâ-hu-chō RS ê siang-chhiⁿ-hē-thóng kàu-taⁿ iáu kè-sio̍k sán-seng chòng-lē ê po̍k-chà hiān-siōng. Chha-put-to jī-cha̍p-nî chi̍t-kái, siang-chhiⁿ lāi-té ê âng-kū-chhiⁿ to̍h ē tò kàu-gia̍h ê chúi-sò͘-khì-thé kàu i ê seng-phoan pe̍h-é-chhiⁿ, hō͘ i ê piáu-bīn sán-seng chi̍t-kái chhàn-lān ê jia̍t-he̍k-po̍k-chà. In chha-put-to ū gō͘-chheng kng-nî hn̄g. In sán-seng ê sin-seng po̍k-chà hō͘ Siâ-hu-chō RS siang-chhiⁿ-hē-thóng piàn-kng kàu kúi-ā-pōe, iōng ba̍k-chiu to̍h khòaⁿ-ū. Âng-kū-chhiⁿ to̍h tī chit-pak-tô͘ ê chiàⁿ-pêng téng-koân, pe̍h-é-chhiⁿ to̍h tī tò-pêng hit-ê chiok-kng ê khip-chek-pôaⁿ ê tiong-ng. Siang-chhiⁿ hō͘-siong se̍h tùi-hong leh kiâⁿ ê sî-chūn, khì-thé to̍h ùi âng-kū-chhiⁿ cháu-khì pe̍h-é-chhiⁿ. Thian-bûn-ha̍k-ka thui-sǹg, koh cha̍p-bān-nî liáu-āu, chit-ê siang-chhiⁿ-hē-thóng ē tī pe̍h-é-chhiⁿ lúi-chek kàu-gia̍h ê bu̍t-chit. Tán chhiau-kòe Chandrasekhar ke̍k-hān liáu-āu, to̍h ē sán-seng lêng-liōng koh-khah kiông, siōng-bóe chi̍t-kái ê chhiau-sin-seng po̍k-chà. Ùi chit-ko-goe̍h-thâu khai-sí, lí to̍h ē-tàng khòaⁿ-tio̍h Siâ-hu-chō RS koh piàn-chò chiok-kng ê sin-seng po̍k-chà ah.

[KIP] Pe̍h-é-tshinn Siâ-hu-tsō RS po̍k-tsà

Siâ-hu-tsō RS ê siang-tshinn-hē-thóng kàu-tann iáu kè-sio̍k sán-sing tsòng-lē ê po̍k-tsà hiān-siōng. Tsha-put-to jī-tsa̍p-nî tsi̍t-kái, siang-tshinn lāi-té ê âng-kū-tshinn to̍h ē tò kàu-gia̍h ê tsuí-sòo-khì-thé kàu i ê sing-phuan pe̍h-é-tshinn, hōo i ê piáu-bīn sán-sing tsi̍t-kái tshàn-lān ê jia̍t-hi̍k-po̍k-tsà. In tsha-put-to ū gōo-tshing kng-nî hn̄g. In sán-sing ê sin-sing po̍k-tsà hōo Siâ-hu-tsō RS siang-tshinn-hē-thóng piàn-kng kàu kuí-ā-puē, iōng ba̍k-tsiu to̍h khuànn-ū. Âng-kū-tshinn to̍h tī tsit-pak-tôo ê tsiànn-pîng tíng-kuân, pe̍h-é-tshinn to̍h tī tò-pîng hit-ê tsiok-kng ê khip-tsik-puânn ê tiong-ng. Siang-tshinn hōo-siong se̍h tuì-hong leh kiânn ê sî-tsūn, khì-thé to̍h uì âng-kū-tshinn tsáu-khì pe̍h-é-tshinn. Thian-bûn-ha̍k-ka thui-sǹg, koh tsa̍p-bān-nî liáu-āu, tsit-ê siang-tshinn-hē-thóng ē tī pe̍h-é-tshinn luí-tsik kàu-gia̍h ê bu̍t-tsit. Tán tshiau-kuè Chandrasekhar ki̍k-hān liáu-āu, to̍h ē sán-sing lîng-liōng koh-khah kiông, siōng-bué tsi̍t-kái ê tshiau-sin-sing po̍k-tsà. Uì tsit-ko-gue̍h-thâu khai-sí, lí to̍h ē-tàng khuànn-tio̍h Siâ-hu-tsō RS koh piàn-tsò tsiok-kng ê sin-sing po̍k-tsà ah.

[English] Explosions from White Dwarf Star RS Oph

Spectacular explosions keep occurring in the binary star system named RS Ophiuchi. Every 20 years or so, the red giant star dumps enough hydrogen gas onto its companion white dwarf star to set off a brilliant thermonuclear explosion on the white dwarf's surface. At about 5,000 light years distant, the resulting nova explosions cause the RS Oph system to brighten up by a huge factor and become visible to the unaided eye. The red giant star is depicted on the right of the above drawing, while the white dwarf is at the center of the bright accretion disk on the left. As the stars orbit each other, a stream of gas moves from the giant star to the white dwarf. Astronomers speculate that at some time in the next 100,000 years, enough matter will have accumulated on the white dwarf to push it over the Chandrasekhar Limit, causing a much more powerful and final explosion known as a supernova. Starting early this month, RS Oph was again seen exploding in a bright nova.

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