HH 211：當咧形成的恆星 ê 噴射流

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：HH 211: Jets from a Forming Star
• 影像來源：NASA, ESA, CSA, Webb; 資料處理：Tom Ray (DIAS Dublin)
• 台文翻譯：An-Li Tsai (NSYSU)

[漢羅] HH 211：當咧形成的恆星 ê 噴射流

恆星 當 leh 形成 ê 時陣，敢一定會產生噴射流？ 無人知影。 氣體雲會因為 重力收縮，變做 盤仔形，開始自旋。 毋過伊踅傷緊矣，煞予伊無法度繼續形成 原恆星。 理論學家 假設 講，這款自旋，可能會因為噴出噴射流，予伊 ê 轉踅速度變較低。 In 臆--ê，kah 咱知影 ê Herbig-Haro (HH) 天體 有成。 這是一款有噴射流 ê 少年恆星，有當時仔是 足壯觀足華麗--ê。 這張相片 是 最近 Webb 太空望遠鏡 (JWST) tī 紅外線 翕--ê 影像，有翕著一粒當 leh 形成 ê 少年恆星 HH 211 ê 清楚細節。 綴 2 條狹狹 ê 粒子束 方向，咱閣會當看著 tī 星際氣體 內底，去予噴流衝擊 ê 紅色 震波。 HH 211 ê 噴射流，應該會 tī 紲落來 10 萬年 ê 時間內，沓沓仔變光抑是變暗去，嘛會因為按呢改變伊 ê 外形。 這寡 恆星形成 ê 細節研究，會繼續進行落去。

[POJ] HH 211: Tng-teh hêng-sêng ê Hêng-chheⁿ ê Phùn-siā-liû

Hêng-chheⁿ tng leh hêng-sêng ê sî-chūn, kám it-tēng ē sán-seng phùn-siā-liû? Bô lâng chai-iáⁿ. Khì-thé-hûn ē in-ūi tiōng-le̍k siu-sok, piàn-chò pôaⁿ-á hêng, khai-sí chū-soân. M̄-koh i se̍h siuⁿ kín ah, soah hō͘ i bô-hoat-tō͘ kè-sio̍k hêng-sêng goân-hêng-chheⁿ. Lí-lūn ha̍k-ka ká-siat kóng, chit-khoán chū-soân, khó-lêng ē in-ūi phùn-chhut phùn-siā-liû, hō͘ i ê tńg-se̍h sok-tō͘ piàn khah kē. In ioh--ê, kah lán chai-iáⁿ ê Herbig-Haro (HH) thian-thé ū sêng. Che-sī chi̍t-khoán ū phùn-siā-liû ê siàu-liân hêng-chheⁿ, ū-tang-sî-á sī chiok chòng-koan chiok hôa-lē--ê. Chit-tiuⁿ siòng-phìⁿ sī Webb Thài-khong bōng-oán-kiàⁿ (JWST) tī âng-gōa-sòaⁿ hip--ê iáⁿ-siōng, ū hip-tio̍h chi̍t-lia̍p tng leh hêng-sêng ê siàu-liân hêng-chheⁿ HH 211 ê chheng-chhó sè-chiat. Tòe 2 tiâu e̍h-e̍h ê lia̍p-chú-sok hong-hiòng, lán koh ē-tàng khòaⁿ-tio̍h tī seng-chè khì-thé lāi-té, khì hō͘ phùn-liû chhiong-kek ê âng-sek chìn-pho. HH 211 ê phùn-siā-liû, eng-kai ē tī sòa-lo̍h-lâi 10 bān-nî ê sî-kan-lāi, tau̍h-tau̍h-á piàn kng iah-sī piàn àm khì, mā ē in-ūi án-ne kái-piàn i ê gōa-hêng. Chit kóa hêng-chheⁿ hêng-sêng ê sè-chiat gián-kiù, ē kè-sio̍k chìn-hêng lo̍h-khì.

[KIP] HH 211: Tng-teh hîng-sîng ê Hîng-tshenn ê Phùn-siā-liû

Hîng-tshenn tng leh hîng-sîng ê sî-tsūn, kám it-tīng ē sán-sing phùn-siā-liû? Bô lâng tsai-iánn. Khì-thé-hûn ē in-uī tiōng-li̍k siu-sok, piàn-tsò puânn-á hîng, khai-sí tsū-suân. M̄-koh i se̍h siunn kín ah, suah hōo i bô-huat-tōo kè-sio̍k hîng-sîng guân-hîng-tshenn. Lí-lūn ha̍k-ka ká-siat kóng, tsit-khuán tsū-suân, khó-lîng ē in-uī phùn-tshut phùn-siā-liû, hōo i ê tńg-se̍h sok-tōo piàn khah kē. In ioh--ê, kah lán tsai-iánn ê Herbig-Haro (HH) thian-thé ū sîng. Tse-sī tsi̍t-khuán ū phùn-siā-liû ê siàu-liân hîng-tshenn, ū-tang-sî-á sī tsiok tsòng-kuan tsiok huâ-lē--ê. Tsit-tiunn siòng-phìnn sī Webb Thài-khong bōng-uán-kiànn (JWST) tī âng-guā-suànn hip--ê iánn-siōng, ū hip-tio̍h tsi̍t-lia̍p tng leh hîng-sîng ê siàu-liân hîng-tshenn HH 211 ê tshing-tshó sè-tsiat. Tuè 2 tiâu e̍h-e̍h ê lia̍p-tsú-sok hong-hiòng, lán koh ē-tàng khuànn-tio̍h tī sing-tsè khì-thé lāi-té, khì hōo phùn-liû tshiong-kik ê âng-sik tsìn-pho. HH 211 ê phùn-siā-liû, ing-kai ē tī suà-lo̍h-lâi 10 bān-nî ê sî-kan-lāi, ta̍uh-ta̍uh-á piàn kng iah-sī piàn àm khì, mā ē in-uī án-ne kái-piàn i ê guā-hîng. Tsit kuá hîng-tshenn hîng-sîng ê sè-tsiat gián-kiù, ē kè-sio̍k tsìn-hîng lo̍h-khì.

[English] HH 211: Jets from a Forming Star

Do stars always create jets as they form? No one is sure. As a gas cloud gravitationally contracts, it forms a disk that can spin too fast to continue contracting into a protostar. Theorists hypothesize that this spin can be reduced by expelling jets. This speculation coincides with known Herbig-Haro (HH) objects, young stellar objects seen to emit jets -- sometimes in spectacular fashion. Pictured is Herbig-Haro 211, a young star in formation recently imaged by the Webb Space Telescope (JWST) in infrared light and in great detail. Along with the two narrow beams of particles, red shock waves can be seen as the outflows impact existing interstellar gas. The jets of HH 211 will likely change shape as they brighten and fade over the next 100,000 years, as research into the details of star formation continues.

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