Aims.We study the possible atmospheric mass loss from 57 known transiting exoplanets around F, G, K, and M-type stars over evolutionary timescales. For stellar wind induced mass loss studies, we estimate the position of the pressure balance boundary between Coronal Mass Ejection (CME) and stellar wind ram pressures and the planetary ionosphere pressure for non-or weakly magnetized gas giants at close orbits. Methods. The thermal mass loss of atomic hydrogen is calculated by a mass loss equation where we consider a realistic heating efficiency, a radius-scaling law and a mass loss enhancement factor due to stellar tidal forces. The model takes into account the temporal evolution of the stellar EUV flux by applying power laws for F, G, K, and M-type stars. The planetary ionopause obstacle, which is an important factor for ion pick-up escape from non-or weakly magnetized gas giants is estimated by applying empirical power-laws. Results. By assuming a realistic heating efficiency of about 10-25% we found that WASP-12b may have lost about 6-12% of its mass during its lifetime. A few transiting low density gas giants at similar orbital location, like WASP-13b, WASP-15b, CoRoT-1b or CoRoT-5b may have lost up to 1-4% of their initial mass. All other transiting exoplanets in our sample experience negligible thermal loss (≤1%) during their lifetime. We found that the ionospheric pressure can balance the impinging dense stellar wind and average CME plasma flows at distances which are above the visual radius of "Hot Jupiters", resulting in mass losses <2% over evolutionary timescales. The ram pressure of fast CMEs cannot be balanced by the ionospheric plasma pressure for orbital distances between 0.02-0.1 AU. Therefore, collisions of fast CMEs with hot gas giants should result in large atmospheric losses which may influence the mass evolution of gas giants with masses

We studied the interactions between the stellar wind plasma flow of a typical M star, such as GJ 436, and the hydrogen-rich upper atmosphere of an Earth-like planet and a ''super-Earth'' with a radius of 2 R Earth and a mass of 10 M Earth , located within the habitable zone at *0.24 AU. We investigated the formation of extended atomic hydrogen coronae under the influences of the stellar XUV flux (soft X-rays and EUV), stellar wind density and velocity, shape of a planetary obstacle (e.g., magnetosphere, ionopause), and the loss of planetary pickup ions on the evolution of hydrogen-dominated upper atmospheres. Stellar XUV fluxes that are 1, 10, 50, and 100 times higher compared to that of the present-day Sun were considered, and the formation of high-energy neutral hydrogen clouds around the planets due to the charge-exchange reaction under various stellar conditions was modeled. Charge-exchange between stellar wind protons with planetary hydrogen atoms, and photoionization, lead to the production of initially cold ions of planetary origin. We found that the ion production rates for the studied planets can vary over a wide range, from *1.0 · 10 25 s -1 to *5.3 · 10 30 s -1 , depending on the stellar wind conditions and the assumed XUV exposure of the upper atmosphere. Our findings indicate that most likely the majority of these planetary ions are picked up by the stellar wind and lost from the planet. Finally, we estimated the long-time nonthermal ion pickup escape for the studied planets and compared them with the thermal escape. According to our estimates, nonthermal escape of picked-up ionized hydrogen atoms over a planet's lifetime within the habitable zone of an M dwarf varies between *0.4 Earth ocean equivalent amounts of hydrogen (EO H ) to < 3 EO H and usually is several times smaller in comparison to the thermal atmospheric escape rates.

The Radio and Plasma Waves (RPW) instrument on the ESA Solar Orbiter mission is described in this paper. This instrument is designed to measure in-situ magnetic and electric fields and waves from the continuous to a few hundreds of kHz. RPW will also observe solar radio emissions up to 16 MHz. The RPW instrument is of primary importance to the Solar Orbiter mission and science requirements since it is essential to answer three of the four mission overarching science objectives. In addition RPW will exchange on-board data with the other in-situ instruments in order to process algorithms for interplanetary shocks and type III langmuir waves detections.

International audienceThe current status of the large decameter radio telescope UTR-2 (Ukrainian T-shaped Radio telescope) together with its VLBI system called URAN is described in detail. By modernization of these instruments through implementation of novel versatile analog and digital devices as well as new observation techniques, the observational capabilities of UTR-2 have been substantially enhanced. The total effective area of UTR-2 and URAN arrays reaches 200 000 m2, with 24 MHz observational bandwidth (within the 8–32 MHz frequency range), spectral and temporal resolutions down to 4 kHz and 0.5 msec in dynamic spectrum mode or virtually unlimited in waveform mode. Depending on the spectral and temporal resolutions and confusion effects, the sensitivity of UTR-2 varies from a few Jy to a few mJy, and the angular resolution ranges from ~ 30 arcminutes (with a single antenna array) to a few arcseconds (in VLBI mode). In the framework of national and international research projects conducted in recent years, many new results on Solar system objects, the Galaxy and Metagalaxy have been obtained. In order to extend the observation frequency range to 8–80 MHz and enlarge the dimensions of the UTR-2 array, a new instrument – GURT (Giant Ukrainian Radio Telescope) – is now under construction. The radio telescope systems described herein can be used in synergy with other existing low-frequency arrays such as LOFAR, LWA, NenuFAR, as well as provide ground-based support for space-based instruments

[1] Occurrence distributions of the auroral kilometric radiation (AKR) and its right-hand extraordinary (R-X ) and left-hand ordinary (L-O) wave modes are determined from polarization measurements on Interball-2 (Auroral). The AKR is much less frequent on the dayside (20% of the observing time) than on the nightside (70%). A bulk of its occurrence extends from invariant latitude of 80 at afternoon hours of MLT to 60 at night hours. Like the nightside AKR, the dayside one is generated through the electron-cyclotron maser instability. This is concluded from domination of the R-X mode on the dayside similarly to the nightside. On the dayside the L-O mode of AKR is roughly three times more frequent (30% of the AKR time) than that on the nightside (10%). At afternoon hours the L-O occurs more frequently at lower invariant latitudes. This is explained by propagation of the L-O mode from nightside sources far beyond the ''horizon'' of the R-X mode. We find two classes of the circular polarization spectra: ''regular,'' with the dominating R-X mode observed in the upper part of the AKR frequency spectrum and the weak L-O mode in its lower part, and patchy ''irregular,'' with different polarizations interwoven randomly over the whole frequency range of AKR. For ''regular'' spectra the L-O/R-X power ratios are between 0.2 and 0.002. For the ''irregular'' ones they are between 1 and 0.01. The ''irregular'' spectra, reported for the first time, are interpreted as due to irregular refraction of the R-X rays on the plasma density fluctuations near the nightside sources. We show also evidence of another component of the AKR observed on the dayside, which arrives from directions of possible dayside sources likely related to the cusp or the low-latitude boundary layers.INDEX TERMS: 2704 Magnetospheric Physics: Auroral phenomena (2407); 2724 Magnetospheric Physics: Magnetopause, cusp, and boundary layers; 6964 Radio Science: Radio wave propagation; 6939 Radio Science: Magnetospheric physics; KEYWORDS: antennas, auroral phenomena, radio wave propagation, wave in plasma, auroral kilometric radiation Citation: Hanasz, J., M. Panchenko, H. de Feraudy, R. Schreiber, and M. M. Mogilevsky, Occurrence distributions of the auroral kilometric radiation ordinary and extraordinary wave modes,

Context. Observed oscillations of coronal loops in extreme ultraviolet (EUV) lines have been successfully used to estimate plasma parameters in the inner corona (<0.2 R 0 , where R 0 is the solar radius). However, coronal seismology in EUV lines fails for higher altitudes because of rapid decrease in line intensity. Aims. We aim to use radio observations to estimate the plasma parameters of the outer solar corona (>0.2 R 0 ). Methods. We used the large Ukrainian radio telescope URAN-2 to observe type IV radio bursts at the frequency range of 8-32 MHz during the time interval of 09:50-12:30 UT on April 14, 2011. The burst was connected to C2.3 flare, which occurred in AR 11190 during 09:38-09:49 UT. The dynamic spectrum of radio emission shows clear quasi-periodic variations in the emission intensity at almost all frequencies. Results. Wavelet analysis at four different frequencies (29 MHz, 25 MHz, 22 MHz, and 14 MHz) shows the quasi-periodic variation of emission intensity with periods of ∼34 min and ∼23 min. The periodic variations can be explained by the first and second harmonics of vertical kink oscillation of transequatorial coronal loops, which were excited by the same flare. The apex of transequatorial loops may reach up to 1.2 R 0 altitude. We derive and solve the dispersion relation of trapped magnetohydrodynamic oscillations in a longitudinally inhomogeneous magnetic slab. The analysis shows that a thin (with width to length ratio of 0.1), dense (with the ratio of internal and external densities of ≥20) magnetic slab with weak longitudinal inhomogeneity of the Alfvén speed may trap the observed oscillations. Seismologically estimated Alfvén speed inside the loop at the height of ∼1 R 0 is ∼1000 km s −1 . The magnetic field strength at this height is estimated as ∼0.9 G. Extrapolation of magnetic field strength to the inner corona gives ∼10 G at the height of 0.1 R 0 . Conclusions. Radio observations can be successfully used for the sounding of the outer solar corona, where EUV observations of coronal loops fail. Therefore, radio seismology of the outer solar corona is complementary to EUV seismology of the inner corona.

[1] Type III radio bursts are intense solar radio emissions generated by beams of energetic electrons injected into the interplanetary medium. They can be routinely observed by the S/Waves instruments on-board the STEREO (Solar Terrestrial Relation Observatory) spacecraft. We describe goniopolarimetric (GP) inversion of a signal measured on non-orthogonal antennas using the Singular Value Decomposition (SVD) technique. This wave propagation analysis can be applied to spectral matrices built from measurements by the High Frequency Receiver (HFR; a part of the S/Waves experiment). We have found an empirical relation between the decomposed spectral matrices and apparent source sizes for waves with a low degree of polarization. Simulations of electromagnetic emissions with various senses and degrees of polarization, and source shapes show that SVD gives us reasonable results with respect to the polarization ellipsoid geometry. An error analysis considering inaccuracies of HFR has been performed in order to test the validity of the k-vector direction estimation and the obtained empirical relation. We present a joint observation of a type III radio burst by the STEREO and Wind spacecraft during small separation distances. We obtain consistent results for the k-vector direction and apparent source size using different analysis methods for the measurements of the STEREO and Wind spacecraft. We demonstrate that SVD can be an effective tool for the wave analysis of radio emissions measured on non-orthogonal antennas even with very extended sources.Citation: Krupar, V., O. Santolik, B. Cecconi, M. Maksimovic, X. Bonnin, M. Panchenko, and A. Zaslavsky (2012), Goniopolarimetric inversion using SVD: An application to type III radio bursts observed by STEREO,

[1] A method of the direction finding of auroral kilometric radiation (AKR) sources from board of a spinning spacecraft is presented. It uses relative power densities of radiation received on three orthogonal antennas with the assumption that the AKR is circularly polarized. The method is checked for a case of AKR source location provided by Polrad radio-spectro-polarimeter on board the Interball-2 satellite. Projection of the source location along magnetic field lines coincides with the active auroral arc observed by the Polar UV imager.