The impact of the April 2010 Eyjafjallajökull eruption on the atmosphere composition in Moscow     

A. I. Skorokhod  N. F. Elansky  A. N. Safronov  I. D. Eremina  N. V. Pankratova  N. E. Chubarova 《Journal of Volcanology and Seismology》2016,10(4):263-274

This paper reports a study of the April 2010 Eyjafjallajökull eruption on the atmosphere composition in Moscow. Concentrations of some gases, including sulfur dioxide, were measured at a station operated by Moscow University and the Institute of Atmospheric Physics. The impact of this eruption was felt, not only in the composition of the gaseous medium, but also in that of atmospheric precipitation as sampled and analyzed at the Meteorological Observatory of Moscow University. The NOAA hysplit model was used to carry out forward and backward trajectory analyses. It is shown that the descent of air masses during an anticyclone is a necessary condition for reliable recording of volcanic admixtures by ground-based stations.  相似文献   

On the origin and initial temperature of Jupiter and Saturn     

V.S. Safronov  E.L. Ruskol 《Icarus》1982,49(2):284-296

A two-stage growth of the giant planets, Jupiter and Saturn, is considered, which is different from the model of contraction of large gaseous protoplanets. In the first stage, within a time of ～3 × 10⁷ years in Jupiter's zone and ～2 × 10⁸ years in Saturn's zone, a nucleus forms from condensed (solid) material having the mass, ～10²⁸ g, necessary for the beginning of acceleration. The second stage may gravitating body, and a relatively slow accretion begins until the mass of the planet reaches ～10 m_⊕. Then a rapid accretion begins with the critical radius less than the radius of the Hill lobe, so that the classical formulae for the rate of accretion may be applied. At a mass m > m₁ ≈ 50 m_⊕ accretion proceeds slower than it would according to these formulae. When the planet sweeps out all the gas from its nearest zone of feeding (m = m₂ ≈ 130 m_⊕), the width of the exhausted zone being $\text{～}\text{built1}\text{3}$ of the whole zone of the planet) growth is provided the slow diffusion of gas from the rest of the zone (time scale increases to 10⁵?10⁶ years and more). The process is terminated by the dissipation of the remnants of gas. In Saturn's zone m₁ > m₂ ≈ 30 m_⊕. The initial mass of the gas in Jupiter's zone is estimated. Before the beginning of the rapid accretion about 90% of the gas should have been lost from the solar system, and in the planet's zone less than two Jupiter masses remain. The highest temperature of Jupiter's surface, ≈5000°K, is reached at the stage of rapid accretion, m < 100 m_⊕, when the luminosity of the planet reaches 3 × 10^?3 L_⊙. This favors an effective heating of the inner parts of the accretionary disk and the dissipation of gas from the disk. The accretion of Saturn produced a temperature rise up to 2000?2400° K (at m ≈ 20?25 m_⊕) and a luminosity up to 10^?4 L_⊙.  相似文献   

Erratum to: Izvestiya,Atmospheric and Oceanic Physics,Vol. 48, No. 9, 2012     

E. A. Sharkov  Ya. N. Shramkov  I. V. Pokrovskaya  V. G. Bondur  S. A. Pulinets  S. S. Karimova  O. Yu. Lavrova  D. M. Solov’ev  V. V. Kozoderov  T. V. Kondranin  E. V. Dmitriev  V. P. Kamentsev  A. N. Safronov  E. V. Fokeeva  V. S. Rakitin  L. N. Yurganov  E. I. Grechko 《Izvestiya Atmospheric and Oceanic Physics》2014,50(2):224-224

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