Вариации оптической и инфракрасной прозрачности атмосферы Земли под действием космических лучей и изменение термодинамических параметров атмосферы И.В.Кудрявцев Физико-Технический Институт им А.Ф. Иоффе РАН, С.- Петербург, Россия

High-Pass-Mode (HPM) mass spectra of positive ions, obtained by mass spectrometric measurements in the upper troposphere and additionally 3 modeled spectra for H 2 SO 4 concentrations of 1*10 6, 3*10 6 and 1*10 7 cm -3. Spectrum 1: Reference case, ions up to an m of 400 are present. Spectrum 2: Massive ion event, ions up to a m of 2500 are present (S. Eichkorn et al,2002)

Fig. Mean size distributions for cases satisfying the criteria for recent new particle formation: mid- and high-latitude UT/LS (7 to 13 km), tropical troposphere (7 to 17km) and high-latitude stratosphere (17 to 21km). Results from a simulation of the IIN model after 2-day nucleation evolution are shown for a comparison with the mid- and high-latitude UT/LS case. The model uses _80% of the measured peak noontime PH2SO4 and the other average conditions observed for samples showing the feature of new particle formation (table S1). (Inset) The average size distribution at the mid- and high latitudes for samples showing no recent particle formation. ( Lee et al, 2003)

Fig.2. Comparison of measured and simulated particle- size distributions for two cases: high and low ultrafine particle production. (A) Particle number-size distributions measured over 18 minutes on 25 January 2000 at 11.2 km, latitudes from 59°N to 60°N, and longitudes from 4°E to 6°E (blue circles). Particle size distributions as a function of time as simulated by the IIN model (black curves). The model uses a peak noontime P H2SO4 of 300 cm -3 s -1, corresponding to [OH] of two-thirds of the measured value and a fractional sun exposure of Other input parameters, including a background particle mode, were as measured in flight (table S1). The [H 2 SO 4 ] derived from the model is ~1*10 6 cm -3. (B) Particle-size distributions measured over a 12-minute period on 10 December 1999 at 12.5 km, latitudes from 67°N to 70°N, and longitudes from 19°E to 22°E (red triangles). Particle-size distributions as a function of time as simulated by the IIN model, initialized with parameters measured aboard the aircraft (table S1), (black curves).

Fig. Concentration of particles of aerosol larger that 3 nm in diameter, formed during 3 hours Fig. IR spectrum with enhanced ionisation divided by spectrum from ambient background ionisation, showing areas of enhanced absorption at 12.3 and 9:1 mm (810 and 1095cm -1 ). The absorption at 13 mm is due to CO 2. Absorption bands, likely to be from molecular cluster-ions can be seen at 12.3 and 9:2 mm (815 and 1090cm -1 ) ( Aplin and McPheat, 2005)

Fig. Long-term variations of the solar radiation input δ(SQ) in the geographic latitudinal belt j165±688 (thin line) and of GCR intensity dN (dashed line); the thick line displays the 2-yr running average of δ(ΣQ) S.V. Veretenenko*, M.I. Pudovkin, 1999.

It is possible to separate two steps in the process of generation of NO 3 - ion (G.A.M. Dreschhoff1, …,I.V. Koudriavtsev et al, 1999). At first step the capture of electron by oxygen and nitrogen molecules and origination of O 3 - takes place At second step the interaction between ion O 3 - and molecules NO x takes place. This interaction leads to the origination of the ions NO 3 - and molecules CO 2.

Рис. Временные серии вэйвлетно-фильтрованные в полосе лет (использован базис MHAT). A– кривая 1 – Н1, кривая 2 - июльская температура в континентальной части северной Фенноскандии [Lindholm and Eronen, 2000]; B – кривая 1 – Н1, кривая 2 - средняя температура сезона вегетации в приморской части северной Фенноскандии [Briffa et al., 1992]; (Огурцов,2002)

ОСНОВНЫЕ УРАВНЕНИЯ ;; где W- поток солнечного коротковолнового (видимого) излучения; A. B- потоки инфракрасного излучения, распространяющиеся вниз и вверх; 1, 2 - коэффициенты поглощения видимого и инфракрасного излучения в атмосфере, без учета дополнительного поглощения, вызванного влиянием КЛ ; 1, 2 - описывает дополнительное поглощение видимого и инфракрасного излучения, вызванное влиянием КЛ; E= T 4, - постоянная Стефана-Больцмана; T – температура воздуха; коэффициент f

1) Долговременные вариации прозрачности и распределения температуры в атмосфере. dQ =0 Рис. Распределение температуры в атмосфере

Изменение температуры T=T-T 1 для различных значений поглощающего слоя: =0,005; 2 =0; =0,01; 2 =0; =0,02; 2 =0; =0; 2 =0,025; =0; 2 =0,05; =0; 2 =0,1

Кратковременные вариации прозрачности и распределения температуры в атмосфере

Вариации атмосферного давления

Variations of the mean temperature profiles for the anticyclonic conditions before the SCR burst: 1 - on the key day (t=O): 2 - on the third day (t=+3). (M. I. Pudovkin et al, 1996).