ASTROMETRIC RESEARCH IN UKRAINE AT THE XIX – BEGINNING OF XX CENTURIES

The paper presents the stages of development of astrometric research at the Ukrainian observatories in the ХIХ – beginning of ХХ century. They are related to the establishment of university astronomical observatories in Kyiv (1845), Odessa (1871), Kharkiv (1888). Mykolaiv Naval observatory was founded in 1821 for navigation needs with assistance of Admiral A.S. Greig. The absolute catalogs compiled at the Pulkovo and Mykolaiv Observatories made a significant contribution to the international work of compilation of a FK3 system. Special attention is paid to the scientific activity of the oldest observatory at the territory of Ukraine – the Astronomical observatory of L’viv University (1771). Researches at this observatory were mainly concerned with the field of geodesy and meteorology. Despite the short first period of scientific activity (near 10 years), it gave impetus to some famous scientists. At the last decades of ХIХ century observatory of the L’viv University renewed their activity in astrometry, solar physics, and astrophysics. Southern departments of Pulkovo observatory in Odessa (1899) and Mykolaiv (1912) played an important role in extension of Pulkovo absolute catalogues to the southern hemisphere. Systematic observations of the Sun conducted at these departments contributed to the more precise determination of the position of vernal equinox. In ХIХ century Ukrainian observatories participated in the international programs, such as AGK (Astronomischer Gesellschaft Katalog), the photographic catalog “Carte du Ciel” (France). Among the actual observational programs were surveys of zodiacal stars (M.P.Ditchenko in Kyiv), near-pole stars (V.I.Fabritius, R.P.Fogel, M.P.Ditchenko in Kyiv, L.O.Struve and K.N.Kuz'menko in Kharkiv, I.O.Djukov, L.F.Cherniev in Odessa). In the frame of observations of Bonner Durchmusterung (BD) and its southern continuation, organized by the German Astronomical Society, observations of the equatorial zone were provided by I.E. Kortazzi at Mykolaiv observatory, B.V.Novopashenny at the Astronomical Observatory of Odessa University in 1930s years. Needs of astrophotography lead to the creation of the “Сatalog of the faint stars” project. In 1932 at the First Astrometric Conference in Leningrad, the Pulkovo astronomers Gerasimovich B.P and Dniprovsky M.I. suggested the idea of using eхtragalactic nebulae as the reference objects for determination of the absolute motion of the stars. Among the tasks to be solved at the project was compilation of a general catalogue (KSZ) and a fundamental catalog of faint stars (FKSZ). It was planned to involve all the meridian instruments of the USSR as well as foreign ones, especially in the southern hemisphere. The idea of orientation of the KSZ coordinates system related to the observations of small planets was suggested by B.V.Numerov. Astronomers of Mykolaiv Astronomical Observatory participated in the international part of this project (AGK3R-catalogue). The Poltava gravimetric observatory was founded by A.Ya.Orlov in 1926 to construct a gravity map of the territory of Ukraine and to establish astrometric research, earth tides, and Latitude Service with zenith-telescopes. The main research fields of the Main Astronomical Observatory of the NAS of Ukraine, founded by A.Ya.Orlov in 1944, were related to the positional and photographic astrometry during the first decade of its work. We defined three “genealogical scientific trees” of astrometric schools. Two of them were formed under the leadership of outstanding personalities of the XX century: Prof. Alexander Ya. Orlov (the founder and first director of the Observatory, 1944–1948, 1950–1951), who moved to Kyiv from Poltava, and Prof. Avenir A.Yakovkin (director of the Observatory in 1952–1959), who moved to Kyiv from Kazan. The third genealogical tree has grown from the Pulkovo astronomical school. Formation of main directions of scientific researches and its transformation are also discussed. Keywords: astrometric research, positional astrometry, photographic astrometry, fundamental astrometry.

Human Physiological Parameters Related to Solar and Geomagnetic Disturbances: Data from Different Geographic Regions

It is well known that the various manifestations of space weather can influence a wide range of human activities, from technological systems to human health. Various earlier, as well as more recent multi-disciplinary heliobiological and biometeorological studies have revealed that the human organism is sensitive to environmental physical activity changes and reacts to them through variations of the physiological parameters of the human body. This paper constitutes an overview of the National and Kapodistrian University of Athens investigations in regard to the possible effect of solar, geomagnetic, and cosmic ray activity on human physiological parameters. The Athens Cosmic Ray and Solar Physics Groups collaborated with scientific teams from different countries, statistically processing and analyzing data related to human physiological parameters (such as mean heart rate, arterial systolic, and diastolic pressure), or the number of incidents of different types of cardiac arrhythmias and so forth, in relation to data concerning and describing geomagnetic activity (geomagnetic indices Ap and Dst) and variations in cosmic ray intensity (Forbush decreases and cosmic ray intensity enhancements). In total, four projects were carried out concerning data from different geographical regions (Baku, Azerbaijan; Kosice, Slovakia; Tbilisi, Georgia; Piraeus, Greece), covering different time periods and time scales (daily data or yearly data), and referring to different groups of individuals (selected healthy persons or random persons). The studies concluded with interesting results concerning the possible influence of geomagnetic and cosmic ray activity on the human physiological state.

Fine-grained Solar Flare Forecasting Based on the Hybrid Convolutional Neural Networks*

Improving the performance of solar flare forecasting is a hot topic in the solar physics research field. Deep learning has been considered a promising approach to perform solar flare forecasting in recent years. We first used the generative adversarial networks (GAN) technique augmenting sample data to balance samples with different flare classes. We then proposed a hybrid convolutional neural network (CNN) model (M) for forecasting flare eruption in a solar cycle. Based on this model, we further investigated the effects of the rising and declining phases for flare forecasting. Two CNN models, i.e., M rp and M dp, were presented to forecast solar flare eruptions in the rising phase and declining phase of solar cycle 24, respectively. A series of testing results proved the following. (1) Sample balance is critical for the stability of the CNN model. The augmented data generated by GAN effectively improved the stability of the forecast model. (2) For C-class, M-class, and X-class flare forecasting using Solar Dynamics Observatory line-of-sight magnetograms, the means of the true skill statistics (TSS) scores of M are 0.646, 0.653, and 0.762, which improved by 20.1%, 22.3%, and 38.0% compared with previous studies. (3) It is valuable to separately model the flare forecasts in the rising and declining phases of a solar cycle. Compared with model M, the means of the TSS scores for No-flare, C-class, M-class, and X-class flare forecasting of the M rp improved by 5.9%, 9.4%, 17.9%, and 13.1%, and those of the M dp improved by 1.5%, 2.6%, 11.5%, and 12.2%.

Spectral Evolution of an Eruptive Polar Crown Prominence With IRIS Observations

Prominence eruption is closely related to coronal mass ejections and is an important topic in solar physics. Spectroscopic observation is an effective way to explore the plasma properties, but the spectral observations of eruptive prominences are rare. In this paper we will introduce an eruptive polar crown prominence with spectral observations from the Interface Region Imaging Spectrograph (IRIS), and try to explain some phenomena that are rarely reported in previous works. The eruptive prominence experiences a slow-rise and fast-rise phase, while the line-of-sight motions of the prominence plasma could be divided into three periods: 2 hours before the fast-rise phase, opposite Doppler shifts are found at the two sides of the prominence axis; then, red shifts dominate the prominence gradually; in the fast-rise phase, the prominence gets to be blue-shifted. During the second period, a faint component appears in Mg ii k window with a narrow line width and a large red shift. A faint region is also found in AIA 304Å images along the prominence spine, and the faint region gets darker during the expansion of the spine. We propose that the opposite Doppler shifts in the first period is a feature of the polar crown prominence that we studied. The red shifts in the second period are possibly due to mass drainage during the elevation of the prominence spine, which could accelerate the eruption in return. The blue shifts in the third period are due to that the prominence erupts toward the observer. We suggest that the faint component appears due to the decreasing of the plasma density, and the latter results from the expansion of the prominence spine.

FOCSE: CNES Exploration contributions for Operations and Innovation

<p>In 2017, CNES has enforced its visibility and ambitions in Scientific exploration programs by creating the FOCSE (French Operations Centre for Science and Exploration) center. FOCSE groups all the Science Operations activities, including ground segment development, operations and data valorization for the domains involved in the Scientific exploration including Astrophysics & Fundamental Physics, Planets, Small bodies & Solar Physics and Human Spaceflight (Nutrition, Healthcare, Life Science, …). This gives an advantage increasing synergy and commonalities between the different missions and allowing operational people to focus only on what makes each mission original and specific.</p> <p> </p> <p>FOCSE integrates the CADMOS Centre created in 1993, the COMS (Planets Mission centers), Astronomy & Solar systems mission in order to implement a synergetic merge of science in astronomy, solar systems, microgravity and space exploration (robotic and manned). As an example of synergy, we will present the FOCSE Moons & small bodies facility that will be set up for Cubesats activities within the frame of ESA’s planetary defense HERA mission and also in support to JAXA’s MMX mission. This effort will capitalize on our expertise based on our contributions to Rosetta/Philae and Hayabusa2/Mascot on Mission Analysis and visualizing tools to support Scientific activities. We will also present the Spaceship project that has started in coordination with ESA to contribute to the development of technologies for exploration.</p> <p> </p> <p>More recently, CNES proposes to set up a new innovation Lab facility, based on an immersive and open facility for innovation on exploration technologies. Technologies of interests have been identified and will be developed with our partners and also with new actors, in order to allow dynamic spin in and spin off approaches for Exploration technologies. Thanks to this new facility, CNES will provide technical means to create new, innovative, disruptive systems, gather assets from Research, Universities and Industries (from startup to large industrial group) into the same melting-pot, foster collaboration between partners and CNES experts in all space sciences/technologies and operations and join international network of spaceships.</p> <p> </p> <p>The CNES roadmap on Science is defined, the Technological part of this roadmap will be expanded with new Technological opportunities. The proposed paper will present an overview of the CNES strategy and how we implement it on a kind of “DevOps” approach to accelerate and innovate as much as possible, including also a digital factory platform, with the main idea to federate to the network of French Exploration actors (means and expertise) to enforce synergies with ESA and international partners in order to contribute to future Exploration missions.</p> <p> </p>

A note on the sunspot and prominence records made by Angelo Secchi during the period 1871–1875

Angelo Secchi (1818-1878) was an Italian Jesuit who made relevant scientific contributions in the area of geophysics, meteorology and astrophysics. He was a well-known pioneer in solar physics due to his theories and observations. Secchi published in his book Le Soleil (The Sun) a summary of knowledge about our star in that time. Moreover, he published in this book his sunspot and prominence observations made during the period 1871–1875. In this work, we present a machine-readable version of these observations as well as a preliminary analysis of them.

Future Prospects for Solar EUV and Soft X-Ray Spectroscopy Missions

Future prospects for solar spectroscopy missions operating in the extreme ultraviolet (EUV) and soft X-ray (SXR) wavelength ranges, 1.2–1,600 Å, are discussed. NASA is the major funder of Solar Physics missions, and brief summaries of the opportunities for mission development under NASA are given. Upcoming major solar missions from other nations are also described. The methods of observing the Sun in the two wavelength ranges are summarized with a discussion of spectrometer types, imaging techniques and detector options. The major spectral features in the EUV and SXR regions are identified, and then the upcoming instruments and concepts are summarized. The instruments range from large spectrometers on dedicated missions, to tiny, low-cost CubeSats launched through rideshare opportunities.

Transition region adaptive conduction (TRAC) in multidimensional magnetohydrodynamic simulations

Context. In solar physics, a severe numerical challenge for modern simulations is properly representing a transition region between the million-degree hot corona and a much cooler plasma of about 10 000 K (e.g., the upper chromosphere or a prominence). In previous 1D hydrodynamic simulations, the transition region adaptive conduction (TRAC) method has been proven to capture aspects better that are related to mass evaporation and energy exchange. Aims. We aim to extend this method to fully multidimensional magnetohydrodynamic (MHD) settings, as required for any realistic application in the solar atmosphere. Because modern MHD simulation tools efficiently exploit parallel supercomputers and can handle automated grid refinement, we design strategies for any-dimensional block grid-adaptive MHD simulations. Methods. We propose two different strategies and demonstrate their working with our open-source MPI-AMRVAC code. We benchmark both strategies on 2D prominence formation based on the evaporation–condensation scenario, where chromospheric plasma is evaporated through the transition region and then is collected and ultimately condenses in the corona. Results. A field-line-based TRACL method and a block-based TRACB method are introduced and compared in block grid-adaptive 2D MHD simulations. Both methods yield similar results and are shown to satisfactorily correct the underestimated chromospheric evaporation, which comes from a poor spatial resolution in the transition region. Conclusions. Because fully resolving the transition region in multidimensional MHD settings is virtually impossible, TRACB or TRACL methods will be needed in any 2D or 3D simulations involving transition region physics.

THE NATURE OF THE SOLAR ENERGY SOURCE

In solar physics as a result of studies of solar radiation and solar wind Scientists have raised a number of questions. A modern view of the structure of the Sun according to which its core is reacting thermonuclear fusion and solar luminosity energy from the photosphere, does not provide scientifically based answers to them. The article sets out the preliminary scientific evidence of the hypothesis new solar Luminous Energy Source open cycle low-energy nuclear reactions (LENR), entering the photosphere. Based on the physics of nuclear reactions of this cycle answers to questions raised.