鴟鴞星雲 kah 發出 X 光 ê 高溫恆星

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：The Eagle Nebula with X-ray Hot Stars
• 影像來源：X-光: Chandra: NASA/CXC/SAO, XMM: ESA/XMM-Newton; 紅外線：JWST: NASA/ESA/CSA/STScI, Spitzer: NASA/JPL/CalTech; 可見光：Hubble: NASA/ESA/STScI, ESO; 影像處理：L. Frattare, J. Major, N. Wolk, kah K. Arcand
• 台文翻譯：An-Li Tsai (NCU)

[漢羅] 鴟鴞星雲 kah 發出 X 光 ê 高溫恆星

這个有名 ê 鴟鴞星雲 內底 ê 恆星柱 tī X 光波段看起來會是按怎？ 為著欲揣著答案，NASA ê Chandra X 光衛星天文台 就斟酌 leh 看這个有恆星形成 ê 星際雲山。 結果發現，M16 內底 ê 塗粉柱 本身袂發出傷強 ê X 光，毋過有足濟 細罔細 煞蓋光 ê X 光發射源，變甲足明顯--ê。 這寡發射源就是 這張影像 內底 ê 光點。 這張影像是 Chandra（X 光）、XMM（X 光）、JWST （紅外線）、Spitzer（紅外線）、Hubble（可見光）、kah VLT（可見光）天文台影像資料 ê 合成相片。 啥物 恆星 會製造這寡 X 光，到今猶是一个 研究主題。 有一个假說是認為 in 是 高溫、新形成、低質量 ê 恆星，另外一个假說認為 in 是高溫、較老、懸質量 ê 恆星。 這寡會發出 X 光 ê 高溫恆星 tī 這幅圖內底是四界攏是。 進前 tī 可見光 看著 ê，去 hŏng 揣著 ê 蒸發氣體球 (EGGS)，目前 ê 溫度就無夠懸，無法度發出 X 光。

[POJ] Ba̍h-hio̍h seng-hûn kah hoat-chhut X-kng ê ko-un hêng-chhiⁿ

Chit-ê ū-miâ ê Ba̍h-hio̍h seng-hûn lāi-té ê hêng-chhiⁿ-thiāu tī X-kng pho-tōaⁿ khòaⁿ--khí-lâi ē sī-án-chóaⁿ? Ūi-tio̍h beh chhōe-tio̍h tap-àn, NASA ê Chandra X-kng ūi-chhiⁿ Thian-bûn-tâi to̍h chim-chiok leh khòaⁿ chit-ê ū hêng-chhiⁿ hêng-sêng ê seng-chè hûn-soaⁿ. Kiat-kó hoat-hiān, M̌ lāi-té ê thô͘-hún-thiāu pún-sin bē hoat-chhut siuⁿ kiông ê X-kng, m̄-koh ū chiok chē sè bóng sè soah kài kng ê X-kng hoat-siā goân, piàn-kah chiok bêng-hián--ê. Chit-kóa hoat-siā-goân to̍h sī chit-tiuⁿ iáⁿ-siōng lāi-té ê kng-tiám. Chit-tiuⁿ iáⁿ-siōng sī Chandra (X-kng), XMM (X-kng), JWST (âng-gōa-sòaⁿ), Spitzer (âng-gōa-sòaⁿ), Hubble (khó-kiàn-kng), kah VLT (khó-kiàn-kng) thian-bûn-tâi iáⁿ-siōng chu-liāu ê ha̍p-sêng siòng-phìⁿ. Siáⁿ-mih hêng-chhiⁿ ē chè-chō chit-kóa X-kng, kàu-taⁿ iáu-sī chi̍t-ê gián-kiù chú-tê. Ū chi̍t-ê ká-soat jīn-ûi sī ko-un, sin hêng-sêng, kē chit-liōng ê hêng-chhiⁿ, lēng-gōa chi̍t-ê ká-soat jīn-ûi in sī ko-un, khah lāu, koân chit-liōng ê hêng-chhiⁿ. Chit-kóa ē hoat-chhut X-kng ê ko-un hêng-chhiⁿ tī chit-pak tô͘ lāi-té sī sì-kè lóng sī. Chìn-chêng tī khó-kiàn-kng khòaⁿ--tio̍h--ê, khì hőng chhōe-tio̍h ê Chin-hoat Khì-thé-kiû (EGGS), bo̍k-chêng ê un-tō͘ tiō bô-kàu koân, bô-hoat-tō͘ hoat-chhut X-kng.

[KIP] Ba̍h-hio̍h sing-hûn kah huat-tshut X-kng ê ko-un hîng-tshinn

Tsit-ê ū-miâ ê Ba̍h-hio̍h sing-hûn lāi-té ê hîng-tshinn-thiāu tī X-kng pho-tuānn khuànn--khí-lâi ē sī-án-tsuánn? Uī-tio̍h beh tshuē-tio̍h tap-àn, NASA ê Chandra X-kng uī-tshinn Thian-bûn-tâi to̍h tsim-tsiok leh khuànn tsit-ê ū hîng-tshinn hîng-sîng ê sing-tsè hûn-suann. Kiat-kó huat-hiān, M16 lāi-té ê thôo-hún-thiāu pún-sin bē huat-tshut siunn kiông ê X-kng, m̄-koh ū tsiok tsē sè bóng sè suah kài kng ê X-kng huat-siā guân, piàn-kah tsiok bîng-hián--ê. Tsit-kuá huat-siā-guân to̍h sī tsit-tiunn iánn-siōng lāi-té ê kng-tiám. Tsit-tiunn iánn-siōng sī Chandra (X-kng), XMM (X-kng), JWST (âng-guā-suànn), Spitzer (âng-guā-suànn), Hubble (khó-kiàn-kng), kah VLT (khó-kiàn-kng) thian-bûn-tâi iánn-siōng tsu-liāu ê ha̍p-sîng siòng-phìnn. Siánn-mih hîng-tshinn ē tsè-tsō tsit-kuá X-kng, kàu-tann iáu-sī tsi̍t-ê gián-kiù tsú-tê. Ū tsi̍t-ê ká-suat jīn-uî sī ko-un, sin hîng-sîng, kē tsit-liōng ê hîng-tshinn, līng-guā tsi̍t-ê ká-suat jīn-uî in sī ko-un, khah lāu, kuân tsit-liōng ê hîng-tshinn. Tsit-kuá ē huat-tshut X-kng ê ko-un hîng-tshinn tī tsit-pak tôo lāi-té sī sì-kè lóng sī. Tsìn-tsîng tī khó-kiàn-kng khuànn--tio̍h--ê, khì hőng tshuē-tio̍h ê Tsin-huat Khì-thé-kiû (EGGS), bo̍k-tsîng ê un-tōo tiō bô-kàu kuân, bô-huat-tōo huat-tshut X-kng.

[English] The Eagle Nebula with X-ray Hot Stars

What do the famous Eagle Nebula star pillars look like in X-ray light? To find out, NASA's orbiting Chandra X-ray Observatory peered in and through these interstellar mountains of star formation. It was found that in M16 the dust pillars themselves do not emit many X-rays, but a lot of small-but-bright X-ray sources became evident. These sources are shown as bright dots on the featured image which is a composite of exposures from Chandra X-rays, XMM (X-rays), JWST infrared, Spitzer (infrared), Hubble visible, and the VLT (visible). What stars produce these X-rays remains a topic of research, but some are hypothesized to be hot, recently-formed, low-mass stars, while others are thought to be hot, older, high-mass stars. These X-ray hot stars are scattered around the frame -- the previously identified Evaporating Gaseous Globules (EGGS) seen in visible light are not currently hot enough to emit X-rays.

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