Keck near-infrared observations of Saturn's E and G rings during Earth's ring plane crossing in August 1995     

Imke de Pater  Shuleen Chau Martin 《Icarus》2004,172(2):446-454

We present near-infrared (1.24-2.26 μm) images of Saturn's E and G rings which were taken with the W.M. Keck telescope in 1995 August 9-11, during the period that Earth crossed Saturn's ring plane. Our data confirm that the E ring is very blue. Its radial and vertical structure are found to be remarkably similar to that apparent in the HST ringplane crossing data at visible wavelengths, reinforcing models of the ring's peculiar narrow or very steep particle size distribution. Our data show unambiguously that the satellite Tethys is a secondary source of material for the E ring. The G ring is found to be distinctly red, similar in color to Jupiter's main ring, indicative of a (more typical) broad particle size distribution.  相似文献   

A high-resolution infrared spectral survey of Comet C/1999 H1 Lee     

Neil Dello Russo  Michael J. Mumma  Karen Magee-Sauer  Boncho P. Bonev  I.S. McLean 《Icarus》2006,184(1):255-276

We obtained high-resolution (λ/Δλ∼25,000) spectra of Comet C/1999 H1 (Lee) on UT 1999 August 19.6 and 21.6 using the cross-dispersed Near InfraRed SPECtrometer (NIRSPEC) at the Keck Observatory atop Mauna Kea, HI. Here we present spectra of Comet Lee between 2.874 and 3.701 μm (3479-2702 cm⁻¹) representing the most complete high-resolution infrared survey of a comet to date in this wavelength region. Using published line lists and laboratory spectra we have identified 444 of the 545 distinct emission features present in these spectra. We have tabulated the rest frequencies, assignments, relative intensities, and signal-to-noise ratios of all detected emissions. In addition to gaining insights into the chemistry of Comet Lee, this survey provides a valuable tool for planning future high-resolution infrared observations of comets and other astronomical targets, and for retrospective comparison to existing high-resolution infrared datasets.  相似文献   

印度洋dipole事件的年际变化与ENSO事件的联系     

刘琳于卫东  刘玉国 《广东海洋大学学报》2006,26(3):50-55

通过对nino3指数和DMI序列的分析，发现两种物理现象都有4a左右的主要周期，而且印度洋偶极子事件还存在有2a左右的振荡周期，而厄尔尼诺事件在2a时间尺度上周期性不明显；对nino3指数和DMI进行年际时间尺度滤波，结果表明，在年际时间尺度上，两者的相关性比未滤波时有了一定的提高；对年际滤波之后的偶极子事件和ELNINO事件的相关分析可以发现，ELNINO对于印度洋偶极子事件的影响要大于IOD对于太平洋ENSO事件，显示了两者物理现象的影响不对称。  相似文献   

A temperature inversion in "Chinese Arctic Research Expedition 1999   总被引：3，自引：1，他引：2  

刘宇  周立波  邹捍 《极地研究(英文版)》2002,13(1)

1　ＩｎｔｒｏｄｕｃｔｉｏｎＴｈｅＡｒｃｔｉｃａｒｅａ ,ａｓｔｈｅｂａｃｋｇｒｏｕｎｄｏｆｇｌｏｂａｌｃｌｉｍａｔｅａｎｄｅｎｖｉｒｏｎｍｅｎｔ,ｄｒａｗｓｐｅｏ ｐｌｅ’ｓａｔｔｅｎｔｉｏｎｗｉｔｈｉｔｓｉｍｐａｃｔｏｎｇｌｏｂａｌｃｈａｎｇｅ (ＩＰＣＣ 1 990 ) .Ｇｒｅａｔａｍｏｕｎｔｏｆｅｎｅｒｇｙａｎｄｍａｓｓａｒｅｅｘｃｈａｎｇｅｄｂｅｔｗｅｅｎｔｈｅｓｅａａｎｄａｉｒｗｉｔｈｓｐｅｃｉａｌｉｎｔｅｒｆａｃｅ,ａｉｒ ｉｃｅ ｓｅａｓｕｒｆａｃｅ ,ｉｎｔｈｉｓａｒｅａ .Ｔｈｅｒｅｆｏｒｅｉｔｉ…  相似文献   

The 2.9-4.2 micron spectrum of Saturn: Clouds and CH₄, PH₃, and NH₃     

Sang J. Kim  T.R. Geballe 《Icarus》2005,179(2):449-458

We have used synthetic spectra to analyze a medium resolution 2.9-4.2 μm spectrum of Saturn's temperate region observed at UKIRT using CGS4. The synthetic spectra include CH₄, PH₃, and NH₃ lines, for which mixing ratios were adopted from recent Cassini results. The observed absorption features in the spectrum are well accounted for by lines of these molecular species formed 22 +/− 8 km above the 1 bar pressure level at ∼610 mbar. The influence of optically thin haze particles at higher altitudes on the spectrum is not pronounced, with higher spectral resolution probably required to constrain the effects of haze in this wavelength region. Fluorescent line emission by CH₄ in its ν₃ and ν₃+ν₄−ν₄ bands, detected in the 3.2-3.5 μm region, originates between 400 km (∼0.06 mbar) and 800 km (∼0.01 μbar) above the 1 bar level, with peak contributions from the two major contributing bands at 550 km (∼3 μbar) and 700 km (∼0.1 μbar), respectively.  相似文献   

Hydrogen peroxide on Mars: evidence for spatial and seasonal variations     

Th Encrenaz  B Bézard  M.J Richter  S.K Atreya  S Lebonnois  F Forget 《Icarus》2004,170(2):424-429

Hydrogen peroxide (H₂O₂) has been suggested as a possible oxidizer of the martian surface. Photochemical models predict a mean column density in the range of 10¹⁵-10¹⁶ cm⁻². However, a stringent upper limit of the H₂O₂ abundance on Mars (9×10¹⁴ cm⁻²) was derived in February 2001 from ground-based infrared spectroscopy, at a time corresponding to a maximum water vapor abundance in the northern summer (30 pr. μm, Ls=112°). Here we report the detection of H₂O₂ on Mars in June 2003, and its mapping over the martian disk using the same technique, during the southern spring (Ls=206°) when the global water vapor abundance was ∼10 pr. μm. The spatial distribution of H₂O₂ shows a maximum in the morning around the sub-solar latitude. The mean H₂O₂ column density (6×10¹⁵ cm⁻²) is significantly greater than our previous upper limit, pointing to seasonal variations. Our new result is globally consistent with the predictions of photochemical models, and also with submillimeter ground-based measurements obtained in September 2003 (Ls=254°), averaged over the martian disk (Clancy et al., 2004, Icarus 168, 116-121).  相似文献   

Standard electrical conductivity of isotropic, homogeneous olivine in the temperature range 1200°-1500°C     

T. J. Shankland  A. G. Duba 《Geophysical Journal International》1990,103(1):25-31

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Mapping of Io's thermal radiation by the Galileo photopolarimeter-radiometer (PPR) instrument   总被引：1，自引：0，他引：1  

J.A. Rathbun  J.R. Spencer  T.Z. Martin  L.D. Travis 《Icarus》2004,169(1):127-139

Between 1999 and 2002, the Galileo spacecraft made 6 close flybys of Io during which many observations of Io's thermal radiation were made with the photopolarimeter-radiometer (PPR). While the NIMS instrument could measure thermal emission from hot spots with T>200 K, PPR was the only Galileo instrument capable of mapping the lower temperatures of older, cooling lava flows, and the passive background. We tabulate all data taken by PPR of Io during these flybys and describe some scientific highlights revealed by the data. The data include almost complete coverage of Io at better than 250 km resolution, with extensive regional coverage at higher resolutions. We found a modest poleward drop in nighttime background temperatures and evidence of thermal inertia variations across the surface. Comparison of high spatial resolution temperature measurements with observed daytime SO₂ gas pressures on Io provides evidence for local cold trapping of SO₂ frost on scales smaller than the 60 km resolution of the PPR data. We also calculated the power output from several hot spots and estimated total global heat flow to be about 2.0-2.6 W m⁻². The low-latitude diurnal temperature variations for the regions between obvious hot spots are well matched by a laterally-inhomogeneous thermal model with less than 1 W m⁻² endogenic heat flow.  相似文献   

RELATION　BETWEEN　δ~（18）O　IN　ATMOSPHERIC　PRECIPITATION　AND　TEMPERATURE　AND　PRECIPITATION   总被引：3，自引：0，他引：3  

章新平  施雅风  姚檀栋 《中国地理科学(英文版)》1995,(4)

ＲＥＬＡＴＩＯＮＢＥＴＷＥＥＮδ~（１８）ＯＩＮＡＴＭＯＳＰＨＥＲＩＣＰＲＥＣＩＰＩＴＡＴＩＯＮＡＮＤＴＥＭＰＥＲＡＴＵＲＥＡＮＤＰＲＥＣＩＰＩＴＡＴＩＯＮＺｈａｎｇＸｉｎｐｉｎｇ（章新平）（ＤｅｐａｒｔｍｅｎｔｏｆＧｅｏｇｒａｐｈｙ，ＨｕｎａｎＮｏ?..  相似文献   

活动星系核的多波段能谱及其发射机制──Ⅱ．红外连续辐射能谱     

吴建新  周又元 《天文学报》1995,(3)

本文讨论了１６个红外强ＰＧ类星体的红外辐射能谱。我们假设这些活动星系核的红外谱是由非热辐射机制和尘埃的热辐射共同产生的，通过对红外包的最佳拟合，我们发现大多数ＰＧ类星体的红外包位于７一２４μ的中远红外区，尘埃的热辐射机制能很好地产生观测到的红外包。通过模拟能定量地说明尘埃产生的热致辐射在这些天体的红外谱中的相对重要性，在模型与观测值之间的拟合中，我们得到了在这些天体中核加热的尘埃区的大小、尘埃的分布等模型参数。  相似文献