NSF Young Investigator: Evolution of Planetary Atmospheres

NSF 青年研究员:行星大气的演化

基本信息

  • 批准号:
    9457457
  • 负责人:
  • 金额:
    $ 27.5万
  • 依托单位:
  • 依托单位国家:
    美国
  • 项目类别:
    Continuing Grant
  • 财政年份:
    1994
  • 资助国家:
    美国
  • 起止时间:
    1994-07-15 至 1999-12-31
  • 项目状态:
    已结题

项目摘要

9457457 Griffith The origin and evolution of planetary atmospheres will be investigated by focusing initially on two processes: cometary impacts and the greenhouse effect. Collisions of comets and asteroids with planets have recently been found to significantly shape the nature of the solar system. These impacts provide the best explanation for the existence of the moon, Uranus' tilt and the KT extinction. Pioneering work by Zahnle et al (1992) suggests that cometary impact explains the reason why Titan has an atmosphere and the Galilean satellites have none. The idea is that, because of Jupiter's greater mass, impact velocities are larger on the Galilean satellites than on Titan, and thus more efficient at eroding the atmospheres. Monte Carlo calculations that address the stochastic nature of the problem will be used to investigate this effect more rigorously. This technique will also be used to investigate the capability of Mars to retain volatiles. The ultimate goal is to determine the effect that planetary rubble has on a planetary atmosphere as a function of a planet's size and its context within a solar system. This research will address the following question: for a given planetary system, on which bodies might one expect to find an atmosphere? Dr. Griffith will pursue complementary work, at NASA's Infrared Telescope Facility, as a member of the science team that will observe comet Shoemaker-Levy's collision with Jupiter. The aim here is, in part, to investigate how the impact energy is partitioned into chemical energy and kinetic energy to the atmosphere. The partitioning into kinetic energy determines the efficiency with which comets erode planetary atmsopheres. The temperature at Venus' surface is 7500 K, almost 4000 K warmer than the Earth. The great efficiency with which the greenhouse effect warms Venus'atmosphere suggests that warm atmospheres would exist at large distances from the Sun, if greenhouse gases were present. This ra ises an interesting possibility for the ecosphere of the Solar System, that is, the region where liquid water exists, a necessary ingredient for life. Greenhouse gases, if present on a planetary body, may extend the ecosphere out to large distances from the Sun. This possibility will be investigated by focusing on Titan's organic-rich atmosphere. Titan's atmosphere may have originally consisted of ammonia (NH3 ultra violet radiation, a strong greenhouse gas) and subsequently been dissociated by solar on the nitrogen gas (N2) we presently observe. In collaboration with Chris McKay, Kevin Zahnle and Jim Pollack (NASA Ames Research Center), the possibility that Titan's atmosphere was warm enough to have had liquid water in the past will be investigated. This effort will be extended to consider the greenhouse efficiency of the highly abundant volatiles in the solar system (of which, governed by cosmic abundances, there are few). The larger aim of this project is to understand the thermal properties of atmospheres as a function of their composition. This award is to recognize an outstanding young faculty member in science and engineering. The award will enhance the career of the faculty member by providing flexible support for research and educational activities. Cooperation with industry and institutions that support research and education is encouraged.
9457457格里菲斯行星大气的起源和演化将首先集中在两个过程上:彗星撞击和温室效应。最近发现,彗星和小行星与行星的碰撞极大地影响了太阳系的性质。这些撞击为月球的存在、天王星的倾斜和KT的灭绝提供了最好的解释。Zahnle等人(1992)的开创性工作表明,彗星撞击解释了为什么泰坦有大气层,而伽利略卫星没有大气层。这个想法是,由于木星的质量更大,伽利略卫星上的撞击速度比土卫六上的大,因此在侵蚀大气层方面更有效。解决问题的随机性质的蒙特卡罗计算将被用来更严格地研究这种影响。这项技术还将用于研究火星保留挥发物的能力。最终目标是确定行星碎片对行星大气的影响,这是行星大小及其在太阳系中的背景的函数。这项研究将解决以下问题:对于一个给定的行星系统,人们可能会在哪些天体上找到大气层?格里菲斯博士将作为观察苏梅克-利维彗星与木星碰撞的科学团队的一员,在NASA的红外望远镜设施继续进行补充工作。这里的目的在一定程度上是为了研究撞击能量如何被划分为化学能和大气动能。动能的分配决定了彗星侵蚀行星大气的效率。金星表面的温度为7500 K,几乎比地球高4000 K。温室效应使金星大气变暖的巨大效率表明,如果存在温室气体,温暖的大气将存在于距离太阳很远的地方。这为太阳系生态圈带来了一种有趣的可能性,即存在液态水的区域,液态水是生命的必要成分。温室气体如果存在于行星体上,可能会将生态圈延伸到离太阳很远的地方。这种可能性将通过关注土卫六富含有机物质的大气层来进行研究。土卫六的大气层最初可能由氨(NH3紫外线辐射,一种强烈的温室气体)组成,随后被太阳活动分解成我们现在观测到的氮气(氮气)。在克里斯·麦凯、凯文·赞勒和吉姆·波拉克(NASA艾姆斯研究中心)的合作下,泰坦的大气温度足够高,过去存在液态水的可能性将被调查。这一努力将扩展到考虑太阳系中高度丰富的挥发物的温室效应(其中,受宇宙丰富度控制的挥发物很少)。这个项目的更大目标是了解大气的热性质作为其组成的函数。这一奖项是为了表彰一位杰出的科学和工程领域的年轻教员。该奖项将通过为研究和教育活动提供灵活的支持来促进教师的职业生涯。鼓励与支持研究和教育的行业和机构合作。

项目成果

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Caitlin Griffith其他文献

VIMS spectral mapping observations of Titan during the <em>Cassini</em> prime mission
  • DOI:
    10.1016/j.pss.2009.04.013
  • 发表时间:
    2009-12-01
  • 期刊:
  • 影响因子:
  • 作者:
    Jason W. Barnes;Jason M. Soderblom;Robert H. Brown;Bonnie J. Buratti;Christophe Sotin;Kevin H. Baines;Roger N. Clark;Ralf Jaumann;Thomas B. McCord;Robert Nelson;Stéphane Le Mouélic;Sebastien Rodriguez;Caitlin Griffith;Paulo Penteado;Federico Tosi;Karly M. Pitman;Laurence Soderblom;Katrin Stephan;Paul Hayne;Graham Vixie
  • 通讯作者:
    Graham Vixie

Caitlin Griffith的其他文献

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{{ truncateString('Caitlin Griffith', 18)}}的其他基金

Spectral Images of Shoemaker-Levy 9 Impact Sites
Shoemaker-Levy 9 撞击地点的光谱图像
  • 批准号:
    9526282
  • 财政年份:
    1995
  • 资助金额:
    $ 27.5万
  • 项目类别:
    Standard Grant

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