Труды сотрудников ИВМ СО РАН

[Text] / H. K. Biernat [et al.] // Planet Space Sci. - 2007. - Vol. 55, Is. 12. - P1793-1803, DOI 10.1016/j.pss.2007.01.006. - Cited References: 28 . - ISSN 0032-0633РУБ Astronomy & Astrophysics

Аннотация: In this paper, the solar wind flow around Venus is modeled as a nondissipative fluid which obeys the ideal magnetohydrodynamic equations extended for mass loading processes. The mass loading parameter is calculated for four different cases, corresponding to solar minimum and maximum XUV flux and to nominal and low solar wind velocity. We get smooth profiles of the field and plasma parameters in the magnetosheath. Based on the results of this flow model, we investigate the occurrence of the Kelvin-Helmholtz (K-H) instability at the equatorial flanks of the ionopause of Venus. By comparing the instability growth time with the propagation time of the K-H wave, we find that the K-H instability can evolve at the ionopause for all four solar wind conditions. (C) 2007 Elsevier Ltd. All rights reserved.


Доп.точки доступа:
Biernat, H.K.; Erkaev, N.V.; Еркаев, Николай Васильевич; Amerstorfer, U.V.; Penz, T.; Lichtenegger, H.I.M.

[Text] / M. L. Khodachenko [et al.] // Planet Space Sci. - 2007. - Vol. 55: Symposium on Exoplanets and Planetary Formation (APR 25-30, 2004, Nice, FRANCE), Is. 5. - P631-642, DOI 10.1016/j.pss.2006.07.010. - Cited References: 63 . - ISSN 0032-0633РУБ Astronomy & Astrophysics

Аннотация: Atmospheric erosion due to CME-caused ion pick-up is investigated here for the first time for short periodic gas giants (so-called "Hot Jupiters") orbiting close to a star, To study the effect of encountering CMEs produced on the inagnetospheres and atmospheres of "Hot Jupiters" we model possible interaction of dense CME plasma with the exoplanet HD209458b (r(pl) = 1.43r(Jup) M(pl) = 0.69 M(jup)), which orbits a 4.0-5.0 Gyr old Sun-like star at a distance of about 0.045 AU. A numerical hydrodynamic model is applied for calculation of the upper atmospheric density and the hydrogen wind of HD209458b Lis a function of planetocentric distance. Taking into account the similarity of HD209458b's host star to Our Sun we use for the study of the ion production and loss rate of H(+) ions the solar CME plasma parameters and apply a numerical test particle model. Tidal-locking of short periodic exoplanets closely located to their host stars should result in weaker intrinsic planetary magnetic moments, as compared to those of the fast rotating Jupiter type planets at much larger orbits. It is shown that in this case the encountering CME plasma can compress the magnetospheric stand-off distance of short periodic "Hot Jupiters" down to the heights Lit which the ionization and pick-LIP of the planetary neutral atmosphere by the CME plasma flow take place. Assuming for the host star of HD209458b the same CME occurrence rate Lis on the Suit, we estimate possible total mass loss rates of HD2094581b due to its collisions with CMEs over the planet lifetime. It has been found that Under different estimations of the value of a planetary magnetic moment, HD209458b Could have lost over its lifetime the mass from 0-2 up to several times of its present mass M(pl). (c) 2006 Elsevier Ltd. All rights reserved.


Доп.точки доступа:
Khodachenko, M.L.; Lammer, H.; Lichtenegger, H.I.M.; Langmayr, D.; Erkaev, N.V.; Еркаев, Николай Васильевич; Griessmeier, J.M.; Leitner, M.; Penz, T.; Biernat, H.K.; Motschmann, U.; Rucker, H.O.

[Text] / H. . Lammer [et al.] // Astrobiology. - 2007. - Vol. 7, Is. 1. - P185-207, DOI 10.1089/ast.2006.0128. - Cited References: 104 . - ISSN 1531-1074РУБ Astronomy & Astrophysics + Biology + Geosciences, Multidisciplinary

Аннотация: Atmospheric erosion Of CO2-rich Earth-size exoplanets due to coronal mass ejection (CME)-induced ion pick up within close-in habitable zones of active M-type dwarf stars is investigated. Since M stars are active at the X-ray and extreme ultraviolet radiation (XUV) wavelengths over long periods of time, we have applied a thermal balance model at various XUV flux input values for simulating the thermospheric heating by photodissociation and ionization processes due to exothermic chemical reactions and cooling by the CO2 infrared radiation in the 15 mu m band. Our study shows that intense XUV radiation of active M stars results in atmospheric expansion and extended exospheres. Using thermospheric neutral and ion densities calculated for various XUV fluxes, we applied a numerical test particle model for simulation of atmospheric ion pick up loss from an extended exosphere arising from its interaction with expected minimum and maximum CME plasma flows. Our results indicate that the Earth-like exoplanets that have no, or weak, magnetic moments may lose tens to hundreds of bars of atmospheric pressure, or even their whole atmospheres due to the CME-induced O+ ion pick up at orbital distances <= 0.2 astronomical units. We have found that, when exposed to intense XUV fluxes, atmospheres with CO2/N-2 mixing ratios lower than 96% will show an increase in exospheric temperatures and expanded thermosphere-exosphere environments. Hence, they suffer stronger atmospheric erosion, which can result in the total loss of several hundred bars even if an exoplanet is protected by a "magnetic shield" with its boundary located at I Earth radius above the surface. Furthermore, our study indicates that magnetic moments of tidally locked Earth-like exoplanets are essential for protecting their expanded upper atmospheres because of intense XUV radiation against CME plasma erosion. Therefore, we suggest that larger and more massive terrestrial-type exoplanets may better protect their atmospheres against CMEs, because the larger cores of such exoplanets would generate stronger magnetic moments and their higher gravitational acceleration would constrain the expansion of their thermosphere-exosphere regions and reduce atmospheric escape.


Доп.точки доступа:
Lammer, H.; Lichtenegger, H.I.M.; Kulikov, Y.N.; Griessmeier, J.M.; Terada, N.; Erkaev, N.V.; Еркаев, Николай Васильевич; Biernat, H.K.; Khodachenko, M.L.; Ribas, I.; Penz, T.; Selsis, F.

[Text] / M. Blanc, R. Kallenbach, N. V. Erkaev // Space Sci. Rev. - 2005. - Vol. 116: Workshop on Comparative Study of the Outer Planets before the Exploration of Saturn (JAN 12-14, 2004, Bern, SWITZERLAND), Is. 01.02.2013. - P227-298, DOI 10.1007/s11214-005-1958-y. - Cited References: 202 . - ISSN 0038-6308РУБ Astronomy & Astrophysics

Аннотация: This article proposes a short review of our present knowledge of solar system magnetospheres, with the purpose of placing the study of Saturn's inagnetosphere in the context of a comparative approach. We describe the diversity of solar system magnetospheres and the underlying causes of this diversity: nature and magnetization state of the planetary obstacle, presence or not of a dense atmosphere, rotation state of the planet, existence of a system of satellites, rings and neutral gas populations in orbit around the planet. We follow the "russian doll" hierarchy of solar system magnetospheres to briefly describe the different objects of this family: the heliosphere, which is the Sun's magnetosphere; the "elementary" magnetospheres of the inner planets, Earth and Mercury; the "complex" magnetospheres of the giant planets, dominated by planetary rotation and the presence of interacting objects within their magnetospheric cavities, some of which, like Ganymede, to or Titan, produce small intrinsic or induced magnetospheres inside the large one. We finally describe the main original features of Saturn's magnetosphere as we see them after the Voyager fly-bys and before the arrival of Cassini at Saturn, and list some of the key questions which Cassini will have to address during its four-year orbital tour.


Доп.точки доступа:
Blanc, M.; Kallenbach, R.; Erkaev, N.V.; Еркаев, Николай Васильевич

[Text] / H. Lammer [et al.] // Planet Space Sci. - 2006. - Vol. 54, Is. 13-14. - P1445-1456, DOI 10.1016/j.pss.2006.04.022. - Cited References: 93 . - ISSN 0032-0633РУБ Astronomy & Astrophysics

Аннотация: Atmospheric escape from the upper atmosphere of Venus is mainly influenced by the loss of hydrogen and oxygen caused by the interaction of solar radiation and particle flux with the unprotected planetary environment. Because one main aim of the ASPERA-4 particle/plasma and VEX-MAG magnetic field experiments on board of ESA's forthcoming Venus Express mission is the investigation of atmospheric erosion processes from the planet's ionosphere-exosphere environment, we study the total loss of hydrogen and oxygen and identified the efficiency of several escape mechanisms involved. For the estimation of pick up loss rates we use a gas dynamic test particle model and obtained average loss rates for H+, and O+ pick up ions of about 1 x 10(25) s(-1) and about 1.6 x 10(25) s(-1), respectively. Further, we estimate ion loss rates due to detached plasma clouds, which were observed by the pioneer Venus orbiter and may be triggered by the Kelvin-Helmholtz instability of about 0.5-1 x 10(25) s(-1). Thermal atmospheric escape processes and atmospheric loss by photo-chemically produced oxygen atoms yield negligible loss rates. Sputtering by incident pick up O+ ions give O atom loss rates in the order of about 6 x 10(24) s(-1). On the other hand, photo-chemically produced hot hydrogen atoms are a very efficient loss mechanism for hydrogen on Venus with a global average total loss rate of about 3.8 x 10(25) s(-1), which is in agreement with Donahue and Hartle [1992. Solar cycle variations in H+ and D+ densities in the Venus ionosphere: implications for escape. Geophys. Res. Lett. 12, 2449-2452] and of the same order but less than the estimated H+ ion outflow on the Venus nightside of about 7.0 x 10(25) s(-1) due to acceleration by an outward electric polarization force related to ionospheric holes by Hartle and Grebowsky [1993. Light ion flow in the nightside ionosphere of Venus. J. Geophys. Res. 98, 7437-7445]. Our study indicates that on Venus, due to its larger mass and size compared to Mars, the most relevant atmospheric escape processes of oxygen involve ions and are caused by the interaction with the solar wind. The obtained results indicate that the ratio between H/O escape to space from the Venusian upper atmosphere is about 4, and is in a much better agreement with the stoichiometrically H/O escape ratio of 2:1, which is not the case on Mars. However, a detailed analysis of the outflow of ions from the Venus upper atmosphere by the ASPERA-4 and VEX-MAG instruments aboard Venus Express will lead to more accurate atmospheric loss estimations and a better understanding of the planet's water inventory. (c) 2006 Elsevier Ltd. All rights reserved.


Доп.точки доступа:
Lammer, H.; Lichtenegger, H.I.M.; Biernat, H.K.; Erkaev, N.V.; Еркаев, Николай Васильевич; Arshukova, I.L.; Kolb, C.; Gunell, H.; Lukyanov, A.; Holmstrom, M.; Barabash, S.; Zhang, T.L.; Baumjohann, W.

[Text] / A. P. Gavrilyuk, N. Y. Shaparev // Chin. Phys. B. - 2014. - Vol. 23, Is. 2. - Ст. 25205, DOI 10.1088/1674-1056/23/2/025205. - Cited References: 14 . - ISSN 1674-1056. - ISSN 1741-4199РУБ Physics, Multidisciplinary

Аннотация: In this paper, it is shown that the laser radiation intensity required for complete ionization of vapors produced on an irradiated metal surface can be reduced by more than an order of magnitude through using pulsed laser radiation in combination with microwave radiation.

wos

Держатели документа:
[Gavrilyuk, Anatoli P.
Shaparev, Nikolai Ya] Russian Acad Sci, Siberian Branch, Inst Computat Modeling, Krasnoyarsk, Russia
[Gavrilyuk, Anatoli P.] Siberian Fed Univ, Krasnoyarsk, Russia
ИВМ СО РАН

Доп.точки доступа:
Shaparev, N.Ya.; Шапарев, Николай Якимович; Гаврилюк, Анатолий Петрович

/ A. P. Gavriluk, N. Ya. Shaparev // Opt. Commun. - 1981. - Vol. 39, Is. 6. - P379-382, DOI 10.1016/0030-4018(81)90227-3. - Cited References: 11 . - ISSN 0030-4018РУБ Optics

Аннотация: The propagation of the resonance electromagnetic wave accompanied by gas ionization is considered. Plasma is formed through initial associative processes followed by the action of electrons which gain energy when colliding with the excited atoms. The change in the nature of the radiation propagation results from both a decrease in the ground state atom density and an increase in the probability of the upper state atom de-excitation. Concrete estimates are made for cesium. The degree of gas ionization and the wave propagation velocity of transparency are calculated. В© 1981.

WOS,
Scopus

Держатели документа:
Computing Center of the Siberian Branch of the USSR, Academy of Sciences, Krasnoyarsk, USSR, 660049
ИВМ СО РАН

Доп.точки доступа:
GAVRILUK, A.P.; Гаврилюк, Анатолий Петрович; Shaparev, N.Ya.; Шапарев, Николай Якимович

/ A. P. Gavriluk, N. Ya. Shaparev, O. E. Yakubailik // Qiangjiguang Yu Lizishu/High Power Laser and Particle Beams. - 1994. - Vol. 6, Is. 1. - P91-98 . - ISSN 1001-4322
Аннотация: Theoretical analysis and numerical calculations were performed to investigate the laser impulse coupling to aluminum targets irradiated in vacuum with conduction, vaporization and plasma ignition being taken into consideration. The significant role of a correct description of the vaporization process was shown. It was found also that the two-photon ionization results in the increase of initial electron density and their temperature, and this, in the long run, results in the increase of excited atoms density and the rate of electron origination at the expense of their photoionization grows accordingly. The impulse coupling and plasma ignition threshold data are in good agreement with the experimental results.

Scopus

Держатели документа:
Krasnoyarsk Computing Center of the, Russian Acad of Sciences, Russian Federation
ИВМ СО РАН

Доп.точки доступа:
Shaparev, N.Ya.; Шапарев, Николай Якимович; Якубайлик, Олег Эдуардович; Yakubaylik O.E.; Гаврилюк, Анатолий Петрович

/ A. P. Gavrilyuk // Teplofizika Vysokikh Temperatur. - 1995. - Vol. 33, Is. 1. - P144-146 . - ISSN 0040-3644
Аннотация: The paper assesses coefficients and rates of ionization caused by an electron shock of atomic gas. It is meant that this gas is excited by resonance radiation and that ionization rate depends on the tune out of radiation frequency from the center of absorption line. It has been shown that in the central part of the line, where saturation is implemented, the coefficient depends only on characteristics of the resonance transition and ionization potential of the atom, and that the growth of electron concentration in time is exponential. When the far end of the line is tuned out, saturation disappears and dynamics of concentration growth becomes nonlinear.

Scopus

Держатели документа:
VTs SO RAN, Krasnoyarsk, Russian Federation
ИВМ СО РАН

Доп.точки доступа:
Gavrilyuk, A.P.; Гаврилюк, Анатолий Петрович

/ I. F. Shaikhislamov [et al.] // Astrophys. J. - 2014. - Vol. 795, Is. 2, DOI 10.1088/0004-637X/795/2/132 . - ISSN 0004-637X
Аннотация: In the present series of papers we propose a consistent description of the mass loss process. To study in a comprehensive way the effects of the intrinsic magnetic field of a close-orbit giant exoplanet (a so-called hot Jupiter) on atmospheric material escape and the formation of a planetary inner magnetosphere, we start with a hydrodynamic model of an upper atmosphere expansion in this paper. While considering a simple hydrogen atmosphere model, we focus on the self-consistent inclusion of the effects of radiative heating and ionization of the atmospheric gas with its consequent expansion in the outer space. Primary attention is paid to an investigation of the role of the specific conditions at the inner and outer boundaries of the simulation domain, under which different regimes of material escape (free and restricted flow) are formed. A comparative study is performed of different processes, such as X-ray and ultraviolet (XUV) heating, material ionization and recombination, H+ 3 cooling, adiabatic and Lyα cooling, and Lyα reabsorption. We confirm the basic consistency of the outcomes of our modeling with the results of other hydrodynamic models of expanding planetary atmospheres. In particular, we determine that, under the typical conditions of an orbital distance of 0.05AU around a Sun-type star, a hot Jupiter plasma envelope may reach maximum temperatures up to ∼9000K with a hydrodynamic escape speed of ∼9 km s-1, resulting in mass loss rates of ∼ (4-7) · 1010 g s-1. In the range of the considered stellar-planetary parameters and XUV fluxes, that is close to the mass loss in the energy-limited case. The inclusion of planetary intrinsic magnetic fields in the model is a subject of the follow-up paper (Paper II).

Scopus,
Полный текст (доступен только в локальной сети)

Держатели документа:
Institute of Computational Modelling, SB RASKrasnoyarsk, Russian Federation

Доп.точки доступа:
Shaikhislamov, I.F.; Khodachenko, M.L.; Sasunov, Y.L.; Lammer, H.; Kislyakova, K.G.; Erkaev, N.V.; Еркаев, Николай Васильевич

[Text] / V. Shaydurov, G. Shchepanovskaya, M. Yakubovich ; ed. M. D. Todorov // APPLICATION OF MATHEMATICS IN TECHNICAL AND NATURAL SCIENCES : AMER INST PHYSICS, 2015. - Vol. 1684: 7th International Conference on Application of Mathematics in Technical (JUN 28-JUL 03, 2015, Albena, BULGARIA). - Ст. UNSP 020003. - (AIP Conference Proceedings), DOI 10.1063/1.4934284. - Cited References:23 . - РУБ Mathematics, Applied + Physics, Applied

Аннотация: In the paper, a mathematical model and a numerical algorithm are proposed for modeling the complex of phenomena which accompany the passage of a friable asteroid-comet body through the Earth's atmosphere: the material ablation, the dissociation of molecules, and the radiation. The proposed model is constructed on the basis of the Navier-Stokes equations for viscous heat-conducting gas with an additional equation for the motion and propagation of a friable lumpy-dust material in air. The energy equation is modified for the relation between two its kinds: the usual energy of the translation of molecules (which defines the temperature and pressure) and the combined energy of their rotation, oscillation, electronic excitation, dissociation, and radiation. For the mathematical model of atmosphere, the distribution of density, pressure, and temperature in height is taken as for the standard atmosphere. An asteroid-comet body is taken initially as a round body consisting of a friable lumpy-dust material with corresponding density and significant viscosity which far exceed those for the atmosphere gas. A numerical algorithm is proposed for solving the initial-boundary problem for the extended system of Navier-Stokes equations. The algorithm is the combination of the semi-Lagrangian approximation for Lagrange transport derivatives and the conforming finite element method for other terms. The implementation of these approaches is illustrated by a numerical example.

WOS,
Scopus,
Смотреть статью

Держатели документа:
SB RAS, Inst Computat Modeling, Krasnoyarsk 660036, Russia.
Siberian Fed Univ, Krasnoyarsk 660041, Russia.

Доп.точки доступа:
Shchepanovskaya, G.I.; Щепановская, Галина Ивановна; Yakubovich, M.V.; Якубович, Максим Викторович; Todorov, M.D. \ed.\; Шайдуров, Владимир Викторович

/ N. V. Erkaev [et al.] // Mon. Not. R. Astron. Soc. - 2016. - Vol. 460, Is. 2. - P1300-1309, DOI 10.1093/mnras/stw935 . - ISSN 0035-8711
Аннотация: We investigate the loss rates of the hydrogen atmospheres of terrestrial planets with a range of masses and orbital distances by assuming a stellar extreme ultraviolet (EUV) luminosity that is 100 times stronger than that of the current Sun. We apply a 1D upper atmosphere radiation absorption and hydrodynamic escape model that takes into account ionization, dissociation and recombination to calculate hydrogen mass-loss rates. We study the effects of the ionization, dissociation and recombination on the thermal mass-loss rates of hydrogen-dominated super-Earths and compare the results to those obtained by the energy-limited escape formula which is widely used for mass-loss evolution studies. Our results indicate that the energy-limited formula can to a great extent over- or underestimate the hydrogen mass-loss rates by amounts that depend on the stellar EUV flux and planetary parameters such as mass, size, effective temperature and EUV absorption radius. © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

Scopus,
Смотреть статью,
WOS

Держатели документа:
Institute of Computational Modelling SB RAS, Krasnoyarsk, Russian Federation
Siberian Federal University, Krasnoyarsk, Russian Federation
Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, Graz, Austria
Institute for Astronomy, University of Vienna, Turkenschanzstrasse 17, Vienna, Austria

Доп.точки доступа:
Erkaev, N. V.; Lammer, H.; Odert, P.; Kislyakova, K. G.; Johnstone, C. P.; Gudel, M.; Khodachenko, M. L.

/ V. Shaydurov, G. Shchepanovskaya, M. Yakubovich // (15 June 2016 through 22 June 2016 : Springer Verlag, 2017. - Vol. 10187 LNCS. - P119-131, DOI 10.1007/978-3-319-57099-0_11 . -
Аннотация: In the paper, a mathematical model is proposed for the modeling of the complex of phenomena which accompany the passage of a friable asteroid-comet body through the Earth’s atmosphere: the material ablation, the dissociation of molecules, and the ionization. The model is constructed on the basis of the time-dependent Navier-Stokes equations for viscous heat-conducting gas with an additional equation for the propagation of friable lumpy-dust material in air. A numerical algorithm is proposed for solving the formulated initial boundary-value problem as the combination of the semi-Lagrangian approximation for Lagrange transport derivatives and the conforming finite element method for other terms. A numerical example illustrates these approaches. © Springer International Publishing AG 2017.

Scopus,
Смотреть статью,
WOS

Держатели документа:
Institute of Computational Modeling of Siberian Branch of Russian Academy of Sciences, 50/44 Akademgorodok, Krasnoyarsk, Russian Federation

Доп.точки доступа:
Shchepanovskaya, G.I.; Щепановская, Галина Ивановна; Yakubovich, M.V.; Якубович, Максим Викторович; Шайдуров, Владимир Викторович

/ K. G. Kislyakova [et al.] // Astron. Astrophys. - 2019. - Vol. 623. - Ст. A131, DOI 10.1051/0004-6361/201833941. - Cited References:89. - We acknowledge the support by the Austria Science Fund (FWF) NFN project S116-N16 and the subprojects S11607-N16, S11606-N16 and S11604-N16. P.O., H.L., and N.V.E. acknowledge support from the Austrian Science Fund (FWF) project P25256-N27 "Characterizing Stellar and Exoplanetary Environments via Modeling of Lyman-alpha Transit Observations of Hot Jupiters". N.V.E. also acknowledges support by the RFBR grant No 16-52-14006. M.L.K. also acknowledges FWF projects I2939-N27 and the partial support by the Ministry of Education and Science of Russian federation (Grant No. RFMEFI61617X0084). I.F.S. acknowleges support of Russian Science Foundation project 18-12-00080. The software used in this work was in part developed by the DOE NNSA-ASC OASCR Flash Center at the University of Chicago. This research was conducted using resources provided by the Swedish National Infrastructure for Computing (SNIC) at the High Performance Computing Center North (HPC2N), Umea University, Sweden. The authors are very thankful to Dr. David Ehrenreich for providing the Ly-alpha spectra of GJ 436b, which were used in this article. We would also like to sincerely thank Dr. Vincent Bourrier and Baptiste Lavie for original processing of these spectra. . - ISSN 1432-0746РУБ Astronomy & Astrophysics

Аннотация: Aims. We modeled the transit signatures in the Lyman-alpha (Ly-alpha) line of a putative Earth-sized planet orbiting in the habitable zone (HZ) of the M dwarf GJ 436. We estimated the transit depth in the Ly-alpha line for an exo-Earth with three types of atmospheres: a hydrogen-dominated atmosphere, a nitrogen-dominated atmosphere, and a nitrogen-dominated atmosphere with an amount of hydrogen equal to that of the Earth. For all types of atmospheres, we calculated in-transit absorption they would produce in the stellar Ly-alpha line. We applied it to the out-of-transit Ly-alpha observations of GJ 436 obtained by the Hubble Space Telescope (HST) and compared the calculated in-transit absorption with observational uncertainties to determine if it would be detectable. To validate the model, we also used our method to simulate the deep absorption signature observed during the transit of GJ 436b and showed that our model is capable of reproducing the observations. Methods. We used a direct simulation Monte Carlo (DSMC) code to model the planetary exospheres. The code includes several species and traces neutral particles and ions. It includes several ionization mechanisms, such as charge exchange with the stellar wind, photo- and electron impact ionization, and allows to trace particles collisions. At the lower boundary of the DSMC model we assumed an atmosphere density, temperature, and velocity obtained with a hydrodynamic model for the lower atmosphere. Results. We showed that for a small rocky Earth-like planet orbiting in the HZ of GJ 436 only the hydrogen-dominated atmosphere is marginally detectable with the Space Telescope Imaging Spectrograph (STIS) on board the HST. Neither a pure nitrogen atmosphere nor a nitrogen-dominated atmosphere with an Earth-like hydrogen concentration in the upper atmosphere are detectable. We also showed that the Ly-alpha observations of GJ 436b can be reproduced reasonably well assuming a hydrogen-dominated atmosphere, both in the blue and red wings of the Ly-alpha line, which indicates that warm Neptune-like planets are a suitable target for Ly-alpha observations. Terrestrial planets, on the other hand, can be observed in the Ly-alpha line if they orbit very nearby stars, or if several observational visits are available.

WOS,
Смотреть статью,
Scopus,
РИНЦ

Держатели документа:
Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria.
Austrian Acad Sci, Space Res Inst, Schmiedlstr 6, A-8042 Graz, Austria.
Swedish Inst Space Phys, POB 812, S-98128 Kiruna, Sweden.
Russian Acad Sci, Inst Computat Modelling, Siberian Div, Krasnoyarsk 660036, Russia.
Siberian Fed Univ, Krasnoyarsk, Russia.
Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow, Russia.
Inst Laser Phys SB RAS, Novosibirsk, Russia.

Доп.точки доступа:
Kislyakova, K. G.; Holmstrom, M.; Odert, P.; Lammer, H.; Erkaev, N., V; Khodachenko, M. L.; Shaikhislamov, I. F.; Dorfi, E.; Gudel, M.; Guedel, Manuel; Kislyakova, Kristina; Austria Science Fund (FWF) NFN project [S116-N16, S11606-N16, S11604-N16, S11607-N16]; Austrian Science Fund (FWF) [P25256-N27]; RFBR [16-52-14006]; FWF [I2939-N27]; Ministry of Education and Science of Russian federation [RFMEFI61617X0084]; Russian Science Foundation [18-12-00080]

/ A. S. Fedotova [et al.] // IOP Conference Series: Earth and Environmental Science : Institute of Physics Publishing, 2019. - Vol. 315: International Scientific Conference on Agribusiness, Environmental Engineering and Biotechnologies, AGRITECH 2019 (20 June 2019 through 22 June 2019, ) Conference code: 152072, Is. 4. - Ст. 042017, DOI 10.1088/1755-1315/315/4/042017 . -
Аннотация: The article contains the results of hematological, immunological and chemiluminescent analysis of the functional activity of peripheral blood cells of five-year-old lactating cows from the central regions of the Krasnoyarsk Territory (Siberia, Russia) with different radiation status, at which the radiation doses of animals were 0.02, 0.17 and 0.21 mSv per year. It was established that small doses of radiation at 0.17 mSv per year and 0.21 mSv per year affect hematological parameters, increase the phagocytic activity of blood leukocytes and change the kinetics of the formation of active oxygen forms by blood cells, which is manifested as an increase in the time of formation of the maximum kinetics of spontaneous and activated secondary radicals, reduction of the total production of secondary radicals in the antigenic activation of blood cells in vitro and an increase in the volume of spontaneously produced primary radicals. © 2019 IOP Publishing Ltd. All rights reserved.

Scopus,
Смотреть статью

Держатели документа:
Krasnoyarsk State Agrarian University, 90 Mira ane., Krasnoyarsk, 660049, Russian Federation
Institute of Computational Modeling SB RAS, 50/44 Akademgorodok, Krasnoyarsk, 660036, Russian Federation
ISC Research Center for Extreme States of the Body at the Presidium of the FIC KSC SB RAS, 50/12 Akademgorodok, Krasnoyarsk, 660036, Russian Federation

Доп.точки доступа:
Fedotova, A. S.; Turitsina, E. G.; Makarskaya, G. V.; Tarskikh, S. V.