We report on the first simultaneous observation of an Hα Moreton wave, the corresponding EUV fast coronal waves, and a slow and bright EUV wave (typical EIT wave). Associated with an X6.9 flare that occurred on 2011 August 9 at the active region NOAA 11263, we observed a Moreton wave in the Hα images taken by the Solar Magnetic Activity Research Telescope (SMART) at Hida Observatory of Kyoto University. In the EUV images obtained by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamic Observatory (SDO) we found not only the corresponding EUV fast "bright" coronal wave, but also the EUV fast "faint" wave that is not associated with the Hα Moreton wave. We also found a slow EUV wave, which corresponds to a typical EIT wave. Furthermore, we observed, for the first time, the oscillations of a prominence and a filament, simultaneously, both in the Hα and EUV images. To trigger the oscillations by the flare-associated coronal disturbance, we expect a coronal wave as fast as the fast-mode MHD wave with the velocity of about 570 -800 km s −1 . These velocities are consistent with those of the observed Moreton wave and the EUV fast coronal wave.

Abstract. We have investigated type II radio bursts in the solar corona using data from ground-based radio telescopes (>18 MHz) and from the Radio and Plasma Wave experiment (WAVES) on board the WIND spacecraft (<14 MHz). The wavelength range of the WAVES experiment includes the 2-to 14-MHz band, previously unobserved from space. We found that all 34 coronal type II bursts observed over a period of 18 months (November 1, 1994, to April 30, 1996), decayed within a few solar radii and did not propagate into the interplanetary medium. On the other hand, most of the accompanying type III radio bursts observed by the ground-based instruments were observed to continue into the interplanetary medium as the electron beams propagated freely along open magnetic field lines. Over the same period of time, other instruments on board the WIND spacecraft detected about 18 interplanetary shock candidates, which seem to be unrelated to the coronal type II bursts. This result confirms the idea that the coronal and interplanetary shocks are two different populations and are of independent origin. We reexamine the data and conclusions of Gosling et al. [1976], Munro et al. [1979], and Sheeley et al. [1984] and find that their data are consistent with our result that the coronal type II bursts are due to flares. We also briefly discuss the implications of our result to the modeling studies of interplanetary shocks based on input from coronal type II radio bursts. IntroductionCoronal type II radio bursts have long been known [14qM and McCready, 1950]. On the basis of their slow frequency drifts, they were inferred to be due to the propagation of MHD shocks [Uchida, 1960]. Early statistical studies showed that most type II bursts were associated with relatively small Ha flares [e.g., Wright, 1980]. When the first coronal mass ejection (CME) observations were made by the OSO 7 coronagraph, attempts were made to find the spatial relationships between CMEs and the assumed positions of type II radio bursts in order to look for a shock driver. Stewart et al. [1974a, b] were able to study three of the OSO 7 CMEs in conjunction with type II radio bursts. Assuming a coronal density model, those authors converted the observed drift rate of type II bursts into speeds and compared the estimated heights of the type II bursts with those of the OSO 7 CMEs. They found that the type II burst location was ahead of or in the vicinity of the leading edge of the CME. This led to the conclusion that the shocks responsible for type II bursts were piston driven by the CMEs. However, in another CME event, Kosugi The view of the CME-type II relationship began to change after the launch of the CP coronagraph on the SMM satellite. Using SMM/CP data for the April 27, 1980, CME, Stewart et al. [1982] found that the type II burst was located within the CME loop. On the basis of published comparisons of type II burst positions with leading edges of SMM/CP CMEs, Wagner and MacQueen [1983] proposed that the type II burst is produced by a flare shock, independent ...

rcsponse along lines of Cliver's comments, so each subsection of the comment has a corresponding response. Response to the Counterarguments Type II Bursts Near Solar MaximumSince our data set presented in paper 1 belongs to the solar minimum period, Cliver [

Quantum communication, and more specifically Quantum Key Distribution (QKD), enables the transmission of information in a theoretically secure way, guaranteed by the laws of quantum physics. Although fiber-based QKD has been readily available since several years ago, a global quantum communication network will require the development of space links, which remains to be demonstrated. NICT launched a LEO satellite in 2014 carrying a lasercom terminal (SOTA), designed for in-orbit technological demonstrations. In this paper, we present the results of the campaign to measure the polarization characteristics of the SOTA laser sources after propagating from LEO to ground. The most-widely used property for encoding information in free-space QKD is the polarization, and especially the linear polarization. Therefore, studying its behavior in a realistic link is a fundamental step for proving the feasibility of space quantum communications. The results of the polarization preservation of two highly-polarized lasers are presented here, including the first-time measurement of a linearly-polarized source at λ = 976 nm and a circularly-polarized source at λ = 1549 nm from space using a realistic QKD-like receiver, installed in the Optical Ground Station at the NICT Headquarters, in Tokyo, Japan.