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首页> 外文期刊>The Astrophysical journal >FAR-ULTRAVIOLET SPECTROSCOPY OF VENUS AND MARS AT 4 A RESOLUTION WITH THE HOPKINS ULTRAVIOLET TELESCOPE ON ASTRO-2
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FAR-ULTRAVIOLET SPECTROSCOPY OF VENUS AND MARS AT 4 A RESOLUTION WITH THE HOPKINS ULTRAVIOLET TELESCOPE ON ASTRO-2

机译：霍普金斯紫外线望远镜在ASTRO-2上4 A解析金星和火星的远紫外光谱

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摘要

Far-ultraviolet spectra of Venus and Mars in the range 820-1840 A at ～4 A resolution were obtained on 1995 March 13 and 12, respectively, by the Hopkins Ultraviolet Telescope (HUT), which was part of the Astro-2 observatory on the space shuttle Endeavour. Longward of 1250 A, the spectra of both planets are dominated by emission of the CO fourth positive (A ~1Π—X ~1Σ~+) band system and strong O Ⅰ and C Ⅰ multiplets. In addition, CO Hopfield-Birge bands, B ~1Σ~+ -X ~1Σ~+ (0, 0) at 1151 A and C ~1Σ~+ - X ~1Σ~+ (0, 0) at 1088 A, are detected for the first time, and there is a weak indication of the E ~1Π-X ~1Σ~+ (0, 0) band at 1076 A in the spectrum of Venus. The B-X band is blended with emission from O Ⅰ λ1152. Modeling the relative intensities of these bands suggests that resonance fluorescence of CO is the dominant source of the emission, as it is for the fourth positive system. Shortward of Lyα, other emission features detected include O Ⅱ λ834, O Ⅰ λ989, H Ⅰ Lyβ, and N Ⅰ λλ1134 and 1200. For Venus, the derived disk brightnesses of the O Ⅰ, O Ⅱ, and H Ⅰ features are about one-half of those reported by Hord et al. from Galileo EUV measurements made in 1990 February. This result is consistent with the expected variation from solar maximum to solar minimum. The Ar Ⅰ λλ1048, 1066 doublet is detected only in the spectrum of Mars, and the derived mixing ratio of Ar is of the order of 2%, consistent with previous determinations.
机译：金星和火星的远紫外光谱分别于1995年3月13日和12日在约4 A的分辨率下在820-1840 A范围内获得，该光谱是霍普金斯紫外线望远镜（HUT）组成的。奋进号航天飞机。在1250 A的较长时间内，两个行星的光谱都以CO第四正（A〜1Π-X〜1Σ〜+）带系统的发射以及强的OⅠ和CⅠ多重峰为主。此外，CO Hopfield-Birge频带在1151 A时为B〜1Σ〜+ -X〜1Σ〜+（0，0），在1088 A时为C〜1Σ〜+-X〜1Σ〜+（0，0）首次检测到，并且在金星光谱中1076 A处的E〜1Π-X〜1Σ〜+（0，0）谱带微弱。 B-X波段与OⅠλ1152的发射混合。对这些谱带的相对强度进行建模表明，CO的共振荧光是发射的主要来源，就像第四个阳性系统一样。在Lyα的最短处，检测到的其他发射特征包括OⅡλ834，OⅠλ989，HⅠLyβ和Nλλλ1134和1200。 -Hord等人报道的一半。来自Galileo EUV在1990年2月进行的测量。该结果与从最大太阳到最小太阳的预期变化一致。仅在火星光谱中检测到了ArⅠλλ1048、1066 doublet，与先前的测定结果一致，得出的Ar混合比约为2％。

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