模擬盤仔形星系 ê 形成

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：Simulation: A Disk Galaxy Forms
• 影片來源：TNG Collaboration, MPCDF, FAS Harvard U.; 音樂： World's Sunrise (YouTube: Jimena Contreras)
• 開放科學：Browse 3,000+ codes in the Astrophysics Source Code Library
• 台文翻譯：An-Li Tsai (NCU)

[漢羅] 模擬盤仔形星系 ê 形成

咱是按怎到遮--ê？ 咱知影咱是活 tī 踅恆星 leh 行 ê 行星 頂懸，這粒 恆星 嘛踅一个星系咧行。 毋過這一切是按怎形成 ê 呢？ 因為咱 ê 宇宙 運動速度傷慢矣，咱看袂伊有咧振動抑是無。 所以咱就用電腦模擬較緊 ê 運動速度，來幫贊咱 揣出這个答案。 講較詳細咧，這支影片 是 ùi IllustrisTNG 合作計畫 追蹤 ùi 早期宇宙 (紅移 12) ê 氣體 到 今 (紅移 0) ê 模擬結果。 模擬 拄開始 ê 時陣，規个空間內底 ê 氣體落到 一區相對來講 重力 較懸 ê 部份 累積起來。 等幾若十億年後，這个特殊閣迷人 ê 宇宙舞蹈 會生出一粒較明確 ê 核心。 這內底 ê 氣體丸，有一寡是 較細 ê 衛星星系，in 會繼續落 lŏe 中央，去予 咧轉踅 ê 星系吸收入去。 一直到這支影片結束 ê 時陣，就是到咱這馬 ê 時代。 毋過對 銀河系 來講，大型合併可能猶未結束。 最近 ê 證據表示講，咱這个大型 ê 捲螺仔星系 會 tī 未來幾若十億年內 kah 閣較大型 ê 仙女座 盤仔形捲螺仔星系 相挵。

[POJ] Bô͘-gí Pôaⁿ-á-hêng seng-hē ê Hêng-sêng

Lán sī-án-chóaⁿ kàu chia--ê? Lán chai-iáⁿ lán sī oa̍h tī se̍h hêng-chhiⁿ leh kiâⁿ ê kiâⁿ-chhiⁿ téng-koân, chit-lia̍p hêng-chhiⁿ mā se̍h chi̍t-ê seng-hē leh kiâⁿ. M̄-koh che it-chhè sī án-nóa hêng-sêng ê neh? In-ūi lán ê ú-tiū ūn-tōng sok-tō͘ siuⁿ bān ah, lán khòaⁿ bē-tio̍h i ū teh tín-tāng ia̍h-sī bô. Só͘-í lán to̍h iōng tiān-náu bô͘-gí khah-kín ê ūn-tōng sok-tō͘, lâi pang-chān lán chhōe-chhut chit-ê tap-àn. Kóng khah siông-sè leh, chit-ki iáⁿ-phìⁿ sī ùi IllustrisTNG ha̍p-chok kè-ōe tui-chong ùi chá-kî ú-tiū (âng-î 12) ê khì-thé kàu-taⁿ (âng-î 0) ê bô͘-gí kiat-kó. Bô͘-gí tú-khai-sí ê sî-chūn, kui-ê khong-kan lāi-té ê khì-thé lo̍h kàu chi̍t-khu siong-tùi lâi-kóng tiōng-le̍k khah koân ê pō͘-hūn lúi-chek--khí-lâi. Tán kúi-nā cha̍p-ek nî liáu-āu, chit-ê te̍k-sû koh bê-lâng ê ú-tiū bú-tō ē siⁿ-chhut chi̍t-oân khah bêng-khak ê he̍k-sim. Che lāi-té ê khì-thé-oân, ū chi̍t-kóa sī khah sè ê ūi-chhiⁿ-seng-hē, in ē kè-sio̍k lak-lŏe tiong-ng, khì hō͘ leh tńg-se̍h ê seng-hē khip-siu li̍p-khì. It-ti̍t kàu chit-ki iáⁿ-phìⁿ kiat-sok ê sî-chūn, tio̍h-sī kàu lán chit-má ê sî-tāi. M̄-koh tùi gîrn-hô-hē lâi-kóng, tōa-hêng ha̍p-pèng khó-lêng iáu-bōe kiat-sok. Chòe-kīn ê chèng-kù piáu-sī kóng, lán chit-ê tōa-hêng ê kńg-lê-á seng-hē ē tī bī-lâi kúi-nā cha̍p-ek nî lāi kah koh-khah tōa-hêng ê Sian-lú-chō pôaⁿ-á-hêng kńg-lê-á seng-hē sio-lòng.

[KIP] Bôo-gí Puânn-á-hîng sing-hē ê Hîng-sîng

Lán sī-án-tsuánn kàu tsia--ê? Lán tsai-iánn lán sī ua̍h tī se̍h hîng-tshinn leh kiânn ê kiânn-tshinn tíng-kuân, tsit-lia̍p hîng-tshinn mā se̍h tsi̍t-ê sing-hē leh kiânn. M̄-koh tse it-tshè sī án-nuá hîng-sîng ê neh? In-uī lán ê ú-tiū ūn-tōng sok-tōo siunn bān ah, lán khuànn bē-tio̍h i ū teh tín-tāng ia̍h-sī bô. Sóo-í lán to̍h iōng tiān-náu bôo-gí khah-kín ê ūn-tōng sok-tōo, lâi pang-tsān lán tshuē-tshut tsit-ê tap-àn. Kóng khah siông-sè leh, tsit-ki iánn-phìnn sī uì IllustrisTNG ha̍p-tsok kè-uē tui-tsong uì tsá-kî ú-tiū (âng-î 12) ê khì-thé kàu-tann (âng-î 0) ê bôo-gí kiat-kó. Bôo-gí tú-khai-sí ê sî-tsūn, kui-ê khong-kan lāi-té ê khì-thé lo̍h kàu tsi̍t-khu siong-tuì lâi-kóng tiōng-le̍k khah kuân ê pōo-hūn luí-tsik--khí-lâi. Tán kuí-nā tsa̍p-ik nî liáu-āu, tsit-ê ti̍k-sû koh bê-lâng ê ú-tiū bú-tō ē sinn-tshut tsi̍t-uân khah bîng-khak ê hi̍k-sim. Tse lāi-té ê khì-thé-uân, ū tsi̍t-kuá sī khah sè ê uī-tshinn-sing-hē, in ē kè-sio̍k lak-lue̋ tiong-ng, khì hōo leh tńg-se̍h ê sing-hē khip-siu li̍p-khì. It-ti̍t kàu tsit-ki iánn-phìnn kiat-sok ê sî-tsūn, tio̍h-sī kàu lán tsit-má ê sî-tāi. M̄-koh tuì gîrn-hô-hē lâi-kóng, tuā-hîng ha̍p-pìng khó-lîng iáu-buē kiat-sok. Tsuè-kīn ê tsìng-kù piáu-sī kóng, lán tsit-ê tuā-hîng ê kńg-lê-á sing-hē ē tī bī-lâi kuí-nā tsa̍p-ik nî lāi kah koh-khah tuā-hîng ê Sian-lú-tsō puânn-á-hîng kńg-lê-á sing-hē sio-lòng.

[English] Simulation: A Disk Galaxy Forms

How did we get here? We know that we live on a planet orbiting a star orbiting a galaxy, but how did all of this form? Since our universe moves too slowly to watch, faster-moving computer simulations are created to help find out. Specifically, this featured video from the IllustrisTNG collaboration tracks gas from the early universe (redshift 12) until today (redshift 0). As the simulation begins, ambient gas falls into and accumulates in a region of relatively high gravity. After a few billion years, a well-defined center materializes from a strange and fascinating cosmic dance. Gas blobs -- some representing small satellite galaxies -- continue to fall into and become absorbed by the rotating galaxy as the present epoch is reached and the video ends. For the Milky Way Galaxy, however, big mergers may not be over -- recent evidence indicates that our large spiral disk Galaxy will collide and coalesce with the slightly larger Andromeda spiral disk galaxy in the next few billion years.

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