彗星形雲球

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：Cometary Globules
• 影像來源 kah 版權：Mark Hanson & Martin Pugh, Observatorio El Sauce
• 台文翻譯：An-Li Tsai (NSYSU)

[漢羅] 彗星形雲球

這个無四常 ê 星際結構是啥物？ 這寡 有 明亮邊緣 ê 水流形結構，就 tī 船尾座 kah 船帆座 邊仔附近 ê 豐富星場 內底。 這个星際氣體 kah 塗粉組成 ê 彗星形雲球，是 tī 1300 光年 遠 ê 所在。 是附近高溫恆星發出 ê 高能紫外光輻射，雕出這寡雲球，kā in ê 邊緣離子化，才會發光。 這寡 ùi 船帆座 超新星殘骸 來 ê 雲球，in ê 外形 嘛是 受著 超新星殘骸 ê 影響。 Tī in 內部，冷氣體 kah 塗粉 ê 核心 可能會 崩塌，形成低質量恆星。 這个過程落尾會造成 雲球散去。 事實上，倒爿頂懸 ê 彗星形雲球 CG 30 tī 頭 ê 部份發出暗暗 ê 紅光，這是 恆星形成 早期發出 ê 高能噴射流 造成 ê 現象。

[POJ] Hūi-chhiⁿ-hêng Hûn-kiû

Chit-ê bô sù-siông ê seng-chè kiat-kò͘ sī siáⁿ-mih? Chit kóa ū bêng-liāng pian-iân ê chúi-lâu hêng kiat-kò͘, to̍h tī Chûn-bóe-chō kah Chûn-phâng-chō piⁿ-á hù-kīn ê hong-hù seng-tiûⁿ lāi-té. Chit-ê seng-chè khì-thé kah thô͘-hún cho͘-sêng ê hūi-chhiⁿ-hêng hûn-kiû, sī tī 1300 kng-nî hn̄g ê só͘-chāi. Sī hù-kīn ko-un hêng-chhiⁿ hoat-chhut ê ko-lêng chí-gōa-kng hok-siā, tiau chhut chit kóa hûn-kiû, kā in ê pian-iân lī-chí-hoa, chiah-ē hoat-kng. Chit kóa ùi Chûn-phâng-chō chhiau-sin-seng chân-hâi lâi ê hûn-kiû, in ê gōa-hêng mā-sī siū-tio̍h chhiau-sin-seng chân-hâi ê éng-hióng. Tī in lōe-pō͘, léng khì-thé kah thô͘-hún ê he̍k-sim khó-lêng ē pang-lap, hêng-sêng kē chit-liōng hêng-chhiⁿ. Chit-ê kòe-têng lo̍h-bóe ē chō-sêng hûn-kiû sòaⁿ--khì. Sū-si̍t-siōng, tò-pêng téng-koân ê hūi-chhiⁿ-hêng hûn-kiû CG 30 tī thâu ê pō͘-hūn hoat-chhut àm-àm ê âng-kng, che sī hêng-chhiⁿ hêng-sêng chá-kî hoat--chhut ê ko-lêng phùn-siā-liû chò-sêng ê hiān-siōng.

[KIP] Huī-tshinn-hîng Hûn-kiû

Tsit-ê bô sù-siông ê sing-tsè kiat-kòo sī siánn-mih? Tsit kuá ū bîng-liāng pian-iân ê tsuí-lâu hîng kiat-kòo, to̍h tī Tsûn-bué-tsō kah Tsûn-phâng-tsō pinn-á hù-kīn ê hong-hù sing-tiûnn lāi-té. Tsit-ê sing-tsè khì-thé kah thôo-hún tsoo-sîng ê huī-tshinn-hîng hûn-kiû, sī tī 1300 kng-nî hn̄g ê sóo-tsāi. Sī hù-kīn ko-un hîng-tshinn huat-tshut ê ko-lîng tsí-guā-kng hok-siā, tiau tshut tsit kuá hûn-kiû, kā in ê pian-iân lī-tsí-hua, tsiah-ē huat-kng. Tsit kuá uì Tsûn-phâng-tsō tshiau-sin-sing tsân-hâi lâi ê hûn-kiû, in ê guā-hîng mā-sī siū-tio̍h tshiau-sin-sing tsân-hâi ê íng-hióng. Tī in luē-pōo, líng khì-thé kah thôo-hún ê hi̍k-sim khó-lîng ē pang-lap, hîng-sîng kē tsit-liōng hîng-tshinn. Tsit-ê kuè-tîng lo̍h-bué ē tsō-sîng hûn-kiû suànn--khì. Sū-si̍t-siōng, tò-pîng tíng-kuân ê huī-tshinn-hîng hûn-kiû CG 30 tī thâu ê pōo-hūn huat-tshut àm-àm ê âng-kng, tse sī hîng-tshinn hîng-sîng tsá-kî huat--tshut ê ko-lîng phùn-siā-liû tsò-sîng ê hiān-siōng.

[English] Cometary Globules

What are these unusual interstellar structures? Bright-rimmed, flowing shapes gather near the center of this rich starfield toward the borders of the nautical southern constellations Pupis and Vela. Composed of interstellar gas and dust, the grouping of light-year sized cometary globules is about 1300 light-years distant. Energetic ultraviolet light from nearby hot stars has molded the globules and ionized their bright rims. The globules also stream away from the Vela supernova remnant which may have influenced their swept-back shapes. Within them, cores of cold gas and dust are likely collapsing to form low mass stars, whose formation will ultimately cause the globules to disperse. In fact, cometary globule CG 30 (on the upper left) sports a small reddish glow near its head, a telltale sign of energetic jets from a star in the early stages of formation.

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