HD 163296：恆星形成過程產生 ê 噴流

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：HD 163296: Jet from a Star in Formation
• 影像來源：Visible: VLT/MUSE (ESO); Radio: ALMA (ESO/NAOJ/NRAO)
• 天文物理學家提供：Browse 2,500+ codes in the Astrophysics Source Code Library
• 台文翻譯：An-Li Tsai (NCU)

[漢羅] HD 163296：恆星形成過程產生 ê 噴流

恆星形成 ê 時陣是按怎產生噴流 ê？ 無人有答案。雖然講少年恆星系統 HD 163296 最近 ê 影像敢若有揣著一寡希望。 影像 ê 中心恆星這馬當 leh 形成，毋閣伊已經有 踅伊 leh 行 ê 盤面 kah 噴出 ê 噴流 矣。 這个盤面是用 電波 波段看 ê，是用 tī 智利 ê Atacama 大型次毫米波陣列 (ALMA) 望遠鏡翕--ê。 盤面 ê 溝仔 是 足少年 ê 行星 之間因為重力作用產生 ê。 這个噴流是用 可見光 波段看 ê，嘛是用 tī 智利 ê 超大望遠鏡 (VLT) 翕--ê。 伊 ùi 盤面中心噴出 ê 氣體速度有夠緊 ê，主要 ê 成份是 水素。 這个系統是地球到太陽距離 (AU) ê 幾若百倍。 這寡新 ê 觀測細節會當用來 解說 支持 ê 理論是講，噴流 上無有一部份是 ùi 轉踅 ê 盤面中心 ê 磁場 產生 kah 塑形 ê。 未來 tùi HD 163296 抑是 其他類似 ê 恆星形成系統 ê 觀測，會當幫贊咱了解 in ê 詳細狀況。

[POJ] HD-it-lio̍k-sam-jī-kiú-lio̍k: Hêng-chhiⁿ hêng-sêng kòe-têng sán-seng ê phùn-liû

Hêng-chhiⁿ hêng-sêng ê sî-chūn sī án-ná sán-seng phùn-liû ê? Bô-lâng ū tap-àn. Sui-jiân kóng siàu-liân hêng-chhiⁿ hē-thóng HD-it-lio̍k-sam-jī-kiú-lio̍k chòe-kīn ê iáⁿ-siōng ká-ná ū chhōe-tio̍h chi̍t-kóa hi-bāng. Iáⁿ-siōng ê tiong-sim hêng-chhiⁿ chit-má tng-leh hêng-sêng, m̄-koh i í-keng ū se̍h i leh kiâⁿ ê pôaⁿ-bīn kah phùn-chhut ê phùn-liû ah. Chit-ê pôaⁿ-bīn sī iōng tiān-pho pho-tōaⁿ khòaⁿ--ê, sī iōng tī Tì-lī ê Atacama tōa-hêng chhù-hô-bí-pho tīn-lia̍t (ALMA) bōng-oán-kiàⁿ hip--ê. Pôaⁿ-bīn ê kau-á sī chiok siàu-liân ê kiâⁿ-chhiⁿ chi-kan in-ūi tiōng-le̍k chok-iōng sán-seng ê. Chit-ê phùn-liû sī iōng khó-kiàn-kng pho-tōaⁿ khòaⁿ--ê, mā sī iōng tī Tì-lī ê chhiau-tōa bōng-oán-kiàⁿ (VLA) hip--ê. I ùi pôaⁿ-bīn tiong-sim phùn-chhut ê khì-thé sok-tō͘ ū-kàu kín--ê, chú-iàu ê sêng-hun sī chúi-sò͘. Chit-ê hē-thóng sī Tē-kiû kàu Thài-iông kū-lî (AU) ê kúi-ā-pah poe. Chit-kóa sin--ê koan-chhek sè-chiat ē-tàng iōng-lâi kái-soeh chi-chhî ê lí-lūn sī kóng, phùn-liû siōng-bô ū chi̍t-pō͘-hūn sī ùi tńg-se̍h ê pôaⁿ-bīn tiong-sim ê chû-tiûⁿ sán-seng kah sok-hêng ê. Bī-lâi tùi HD-it-lio̍k-sam-jī-kiú-lio̍k iah-sī kî-tha lūi-sū ê hêng-chhiⁿ hē-thóng ê koan-chhek, ē-tàng pang-chān lán liáu-kái in ê siông-sè chōng-hóng.

[KIP] HD-it-lio̍k-sam-jī-kiú-lio̍k: Hîng-tshinn hîng-sîng kuè-tîng sán-sing ê phùn-liû

Hîng-tshinn hîng-sîng ê sî-tsūn sī án-ná sán-sing phùn-liû ê? Bô-lâng ū tap-àn. Sui-jiân kóng siàu-liân hîng-tshinn hē-thóng HD-it-lio̍k-sam-jī-kiú-lio̍k tsuè-kīn ê iánn-siōng ká-ná ū tshuē-tio̍h tsi̍t-kuá hi-bāng. Iánn-siōng ê tiong-sim hîng-tshinn tsit-má tng-leh hîng-sîng, m̄-koh i í-king ū se̍h i leh kiânn ê puânn-bīn kah phùn-tshut ê phùn-liû ah. Tsit-ê puânn-bīn sī iōng tiān-pho pho-tuānn khuànn--ê, sī iōng tī Tì-lī ê Atacama tuā-hîng tshù-hô-bí-pho tīn-lia̍t (ALMA) bōng-uán-kiànn hip--ê. Puânn-bīn ê kau-á sī tsiok siàu-liân ê kiânn-tshinn tsi-kan in-uī tiōng-li̍k tsok-iōng sán-sing ê. Tsit-ê phùn-liû sī iōng khó-kiàn-kng pho-tuānn khuànn--ê, mā sī iōng tī Tì-lī ê tshiau-tuā bōng-uán-kiànn (VLA) hip--ê. I uì puânn-bīn tiong-sim phùn-tshut ê khì-thé sok-tōo ū-kàu kín--ê, tsú-iàu ê sîng-hun sī tsuí-sòo. Tsit-ê hē-thóng sī Tē-kiû kàu Thài-iông kū-lî (AU) ê kuí-ā-pah pue. Tsit-kuá sin--ê kuan-tshik sè-tsiat ē-tàng iōng-lâi kái-sueh tsi-tshî ê lí-lūn sī kóng, phùn-liû siōng-bô ū tsi̍t-pōo-hūn sī uì tńg-se̍h ê puânn-bīn tiong-sim ê tsû-tiûnn sán-sing kah sok-hîng ê. Bī-lâi tuì HD-it-lio̍k-sam-jī-kiú-lio̍k iah-sī kî-tha luī-sū ê hîng-tshinn hē-thóng ê kuan-tshik, ē-tàng pang-tsān lán liáu-kái in ê siông-sè tsōng-hóng.

[English] HD 163296: Jet from a Star in Formation

How are jets created during star formation? No one is sure, although recent images of the young star system HD 163296 are quite illuminating. The central star in the featured image is still forming but seen already surrounded by a rotating disk and an outward moving jet. The disk is shown in radio waves taken by the Atacama Large Millimeter Array ALMA in Chile, and show gaps likely created by the gravity of very-young planets. The jet, shown in visible light taken by the Very Large Telescope (VLT, also in Chile), expels fast-moving gas -- mostly hydrogen -- from the disk center. The system spans hundreds of times the Earth-Sun distance au. Details of these new observations are being interpreted to bolster conjectures that the jets are generated and shaped, at least in part, by magnetic fields in the rotating disk. Future observations of HD 163296 and other similar star-forming systems may help fill in details.

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