کد مقاله | کد نشریه | سال انتشار | مقاله انگلیسی | نسخه تمام متن |
---|---|---|---|---|
10701324 | 1021128 | 2013 | 31 صفحه PDF | دانلود رایگان |
عنوان انگلیسی مقاله ISI
The thermal structure of Titan's upper atmosphere, I: Temperature profiles from Cassini INMS observations
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موضوعات مرتبط
مهندسی و علوم پایه
علوم زمین و سیارات
علوم فضا و نجوم
پیش نمایش صفحه اول مقاله
![عکس صفحه اول مقاله: The thermal structure of Titan's upper atmosphere, I: Temperature profiles from Cassini INMS observations The thermal structure of Titan's upper atmosphere, I: Temperature profiles from Cassini INMS observations](/preview/png/10701324.png)
چکیده انگلیسی
We derive vertical temperature profiles from Ion Neutral Mass Spectrometer (INMS) N2 density measurements from 32 Cassini passes. We find that the average temperature of Titan's thermosphere varies significantly from pass-to-pass between 112 and 175Â K. The temperatures from individual temperature profiles also varies considerably, with many passes exhibiting wave-like temperature perturbations and large temperature gradients. Wave-like temperature perturbations have wavelengths between 150 and 420Â km and amplitudes between 3% and 22% and vertical wave power spectra of the INMS data and HASI data have a slope between â2 and â3, which is consistent with vertically propagating atmospheric waves. The lack of a strong correlation between temperature and latitude, longitude, solar zenith angle, or local solar time indicates that the thermal structure of Titan's thermosphere is not primarily determined by the absorption of solar EUV flux. At N2 densities greater than 108Â cmâ3, Titan's thermosphere is colder when Titan is observed in Saturn's magnetospheric lobes compared to Saturn's plasma sheet as proposed by Westlake et al. (Westlake, J.H. et al. [2011]. J. Geophys. Res. 116, A03318. http://dx.doi.org/10.1029/2010JA016251). This apparent correlation suggests that magnetospheric particle precipitation causes the temperature variability in Titan's thermosphere; however, at densities smaller than 108Â cmâ3 the lobe passes are hotter than the plasma sheet passes and we find no correlation between the temperature of Titan's thermosphere and ionospheric signatures of enhanced particle precipitation, which suggests that the correlation is not indicative of a physical connection. The temperature of Titan's thermosphere also may have decreased by â¼10Â K around mid-2007. Finally, we classify the vertical temperature profiles to show which passes are hot and cold and which passes have the largest temperature variations. In a companion paper (Part II), we estimate the strength of energy sources and sinks in Titan's thermosphere.
ناشر
Database: Elsevier - ScienceDirect (ساینس دایرکت)
Journal: Icarus - Volume 226, Issue 1, SeptemberâOctober 2013, Pages 552-582
Journal: Icarus - Volume 226, Issue 1, SeptemberâOctober 2013, Pages 552-582
نویسندگان
D. Snowden, R.V. Yelle, J. Cui, J.-E. Wahlund, N.J.T. Edberg, K. Ã
gren,