The physical properties of the “local fluff”

Observations of interstellar gas in front of stars near the Sun are briefly reviewed to obtain for the properties of the local fluff: n−0.1 cm⁻³, n_e^≤ 0.003 cm⁻³, T−11, 500 °K, and B−3−5 μG. The velocity vector obtained from He° λ584 backscattered data (V, 1, b) = (−25 km s⁻¹, 3°, +17°) appears to adequately describe the heliocentric upwind velocity vector for the local fluff.     

What is the threshold amount of starch necessary for full gravitropic sensitivity?

In preparation for microgravity experiments, we studied the kinetics of gravitropism in seedlings of wild-type (WT) Arabidopsis and three starch-deficient mutants. One of these mutants is starchless (ACG 21) while the other two are intermediate starch mutants (ACG 20 and ACG 27). In root cap cells, ACG 20 and 27 have 51% and 60% of the WT amount of starch, respectively. However, in endodermal cells of the hypocotyl, ACG 20 has a greater amount of starch than ACG 27. WT roots and hypocotyls were much more responsive to gravity than were the respective organs of the starchless mutant, and the intermediate starch mutants exhibited reduced gravitropism but had responses that were close to that of the WT. In roots, ACG 27 (more starch) was more responsive than ACG 20 (less starch), while in hypocotyls, ACG 20 (more starch) had a greater response than ACG 27 (less starch). Taken together, our data are consistent with the starch-statolith hypothesis for gravity perception in that the degree of graviresponsiveness is proportional to the total mass of plastids per cell. These results also suggest that (in roots) 51-60% starch is close to the threshold amount of starch needed for full gravitropism and that the gravity sensing system is \"overbuilt.\"     

Living plant systems: How robust are they in the absence of gravity?

The following hierarchical levels can be recognised in plant systems: cells, organs, organisms and gamodemes (interbreeding members of a community). Each level in this ‘living hierarchy’ is both defined and supported by a similar set of sub-systems. Within this framework of plant organization, two complementary questions are relevant for interpreting plant-oriented space experiments: 1) What role, if any, does gravity play in enabling the development of each organizational level? and 2) Does abnormal development in an altered gravity environment indicate sub-system inefficiency? Although a few representatives of the various organizational levels in plant systems have already been the subject of microgravity experiments in space laboratories—from cells in culture to gamodemes, the latter being found in some Closed Environment Life Support Systems—it would be of interest to investigate additional systems with respect to their response to microgravity. Recognition of the sub-systems at each level might be relevant not only for a more complete understanding of plant development but also for the successful cultivation and propagation of plants during long-term space flights and the establishment of plants in extra-terrestrial environments.     

How far are we from a ‘Standard Model’ of the solar dynamo?

Over the last few years, dynamo theorists seem to be converging on a basic scenario as to how the solar dynamo operates. The strong toroidal component of the magnetic field is produced in the tachocline, from where it rises due to magnetic buoyancy to produce active regions at the solar surface. The decay of tilted bipolar active regions at the surface gives rise to the poloidal component, which is first advected poleward by the meridional circulation and then taken below the surface to the tachocline where it can be stretched to produce the toroidal component. The mathematical formulation of this basic model, however, involves the specification of some parameters which are still uncertain. We review these remaining uncertainties which have resulted in disagreements amongst various research groups and have made it impossible to still arrive at something that can be called a standard model of the solar dynamo.     

What is the optimum solar proxy for long-term ionospheric investigations?

The problem of optimum solar proxy is important for long-term and/or climatological studies of ionospheric parameters. Here we focus on possibly different optimum solar proxies for different ionospheric parameters, as they are affected by partly different spectral ranges of solar ionizing radiation. We use yearly average values of foF2 and foE of four European stations with long (1976–2014) and high-quality data (Juliusruh, Pruhonice, Rome, Slough/Chilton), and the global total electron content (G-TEC). Four solar proxies are used: F10.7, Mg II, solar Lymna-alpha flux Fα and sunspot numbers. The most important finding is that the optimum solar proxies are different for different ionospheric parameters. The most suitable solar proxy for foF2 is found to be Mg II, whereas for foE F10.7 evidently outperforms Mg II. Fα and sunspot numbers perform slightly worse but none of four solar proxies performs poorly. F10.7 is favored for G-TEC, to some extent surprisingly, as previous results favored rather Mg II.     

Is the poleward edge of the trough a sensitive indicator of geospace interactions?

The poleward edge of the main ionospheric trough can often be regarded as the ionospheric signature of the equatorward boundary of the plasma sheet. We use Advanced Ionospheric Sounder observations of the poleward edge from Halley, Antarctica (76°S, 27°W; L=4.2) to investigate some aspects of its dynamics with respect to changes of magnetospheric and solar wind conditions. We find that there is frequently rapid equatorward motion of the poleward edge from ∼20 minutes before to ∼30 minutes after the onset of the main phase of a substorm. These observations are discussed in terms of the dynamics of the plasma sheet during substorm activity. Another class of rapid equatorward motion of the poleward edge of the trough has no apparent cause in the magnetosphere or solar wind. Possible explanations involving longitudinal structure of the trough or small-scale structure of the solar wind are considered.     

Where is the base of the Transition Region? Evidence from TRACE,SDO, IRIS and ALMA observations

Classic solar atmospheric models put the Chromosphere-Corona Transition Region (CCTR) at  Mm above the level, whereas radiative MHD (rMHD) models place the CCTR in a wider range of heights. However, observational verification is scarce. In this work we review and discuss recent results from various instruments and spectral domains. In SDO and TRACE images spicules appear in emission in the 1600, 1700 and 304 Å bands and in absorption in the EUV bands; the latter is due to photo-ionization of H i and He i, which increases with wavelength. At the shortest available AIA wavelength and taking into account that the photospheric limb is  Mm above the level, we found that CCTR emission starts at  Mm; extrapolating to , where there is no chromospheric absorption, we deduced a height of  Mm, which is above the value of 2.14 Mm of the Avrett and Loeser model. Another indicator of the extent of the chromosphere is the height of the network structures. Height differences produce a limbward shift of features with respect to the position of their counterparts in magnetograms. Using this approach, we measured heights of  Mm (at 1700 Å),  Mm (at 1600 Å) and  Mm (at 304 Å) for the center of the solar disk. A previously reported possible solar cycle variation is not confirmed. A third indicator is the position of the limb in the UV, where IRIS observations of the Mg ii triplet lines show that they extend up to  Mm above the 2832 Å limb, while AIA/SDO images give a limb height of  Mm (1600 Å) and  Mm (304 Å). Finally, ALMA mm- full-disk images provide useful diagnostics, though not very accurate, due to their relatively low resolution; values of  Mm at 1.26 mm and  Mm at 3 mm were obtained. Putting everything together, we conclude that the average chromosphere extends higher than homogeneous models predict, but within the range of rMHD models..     

Which solar EUV indices are best for reconstructing the solar EUV irradiance?

The solar EUV irradiance is of key importance for space weather. Most of the time, however, surrogate quantities such as EUV indices have to be used by lack of continuous and spectrally resolved measurements of the irradiance. The ability of such proxies to reproduce the irradiance from different solar atmospheric layers is usually investigated by comparing patterns of temporal correlations. We consider instead a statistical approach. The TIMED/SEE experiment, which has been continuously operating since February 2002, allows for the first time to compare in a statistical manner the EUV spectral irradiance to five EUV proxies: the sunspot number, the f10.7, Ca K, and Mg II indices, and the He I equivalent width.     

Are small-scale field-aligned currents and magnetosheath-like particle precipitation signatures of the same low-altitude cusp?

We examined some 75 observations from the low-altitude Earth orbiting DMSP, Ørsted and CHAMP satellites which were taken in the region of the nominal cusp. Our objective was to determine whether the actually observed cusp locations as inferred from magnetosheath-like particle precipitation (“particle cusp”) and intense small-scale magnetic field variations (“current cusp”), respectively, were identical and were consistent with the statistically expected latitude of the cusp derived from a huge number of charged particle spectrograms (“statistical cusp”).     

ISEE-1 and -2 observations of magnetotail flux ropes: FTEs in the plasma sheet?

ISEE-1 and 2 observations from about 20 Re down the near-Earth magnetotail indicate the presence of magnetic flux ropes in the neutral sheet. Magnetic and electric field and fast plasma data show that these structures convect across the spacecraft at speeds of 200–600-km/s, and have scale sizes of roughly 3–5-Re. The rope axis orientation is approximately cross-tail. Their magnetic structure is similar to Venus ionospheric flux ropes, and to flux transfer events at the dayside magnetopause. These structures may arise from patchy reconnection or tearing mode reconnection within the plasma sheet.     

An analysis of the empirical models and the measurement results of the polar atmospheric composition at 120–150 km height

δ = (O/N₂)_exp/(O/N₂)_mod ratios are analysed for the polar thermosphere depending on the season and the heliogeophysical activity where (O/N₂)_exp values are measured at high latitudes with radiofrequency mass spectrometers at MP-12 rocket launchings and (O/N₂)_mod values are calculated for the corresponding conditions of every experiment from 4 models (DTM, MSIS-77, MSIS-83 and Köhnlein model (KL)).The analysis reveals certain regularities in variations for different models. In summer δ_DTM does not depend on the heliogeophysical activity and is within a factor of 2–3 for the polar cap and the daytime cusp at 150 km; during the polar night δ_DTM depends on the geomagnetic disturbance and varies with the solar activity cycle.The δ_MSIS-77 and δ_KL values have little dependence on the heliogeophysical conditions and have approximately the same seasonal variations. During the polar night δ_MSIS-83 corresponds to 1 ± 0.25 at high and low solar activity. The increase in δ dispersion for every model considered is noted at low solar activity in the morning and evening sectors of the auroral oval.     

Is the Earth’s orbital motion linked to the spin rotation of the Sun?

Time variations of the magnetic field of the Sun, seen as a star (the data 1968–2018, with more than 27 thousand daily measurements of the solar mean magnetic field), allowed to specify the rotation period of the gravitating solar mass: 27.027(6)?days, synodic. This indicates a presumably unknown physical connection between motions of the Sun and the Earth: in the course of a year our star accomplishes nearly 27 half-revolutions, while the planet itself performs an identical number of its spinnings during one complete axial revolution of the Sun. True origin of this strange Sun–Earth resonance is unknown, but it is supposed the phenomenon might be caused by slight coherent perturbations of gravity within the solar system.     

Introduction to the Payloads and the Initial Observation Results of Chang＇E-1

Chang'E-1,the orbiter circling the moon 200km above the moon surface,is the first Chinese Lunar exploration satellite.The satellite was successfully launched on 24th October 2007.There are 8 kinds of scientific payloads onboard,including the stereo camera,the laser altimeter,the Sagnac-based interferometer image spectrometer,the Gamma ray spectrometer,the X-ray spectrom-eter,the microwave radiometer,the high energy particle detector,the solar wind plasma detector and a supporting payload data management system.Chang'E-1 opened her eyes to look at the moon and took the first batch of lunar pictures after her stereo camera was switched on in 20th November 2007.Henceforth all the instruments are successfully switched on one by one.After a period of parameter adjustment and initial check out,all scientific instruments are now in their normal operating phase.In this paper,the payloads and the initial observation results are introduced.     

Can a double component outflow explain the X-ray and optical lightcurves of Swift Gamma-Ray Bursts?

An increasing sample of Gamma-Ray Bursts (GRBs) observed by Swift show evidence of ‘chromatic breaks’, i.e. breaks that are present in the X-ray but not in the optical. We find that in a significant fraction of these GRB afterglows the X-ray and the optical emission cannot be produced by the same component. We propose that these afterglow lightcurves are the result of a two-component jet, in which both components undergo energy injection for the whole observation and the X-ray break is due to a jet break in the narrow outflow. Bursts with chromatic breaks also explain another surprising finding, the paucity of late achromatic breaks. We propose a model that may explain the behaviour of GRB emission in both X-ray and optical bands. This model can be a radical and noteworthy alternative to the current interpretation for the ‘canonical’ XRT and UVOT lightcurves, and it bears fundamental implications for GRB physics.     

Experimental and mathematical model of the interactions in the mixed culture of links in the “producer–consumer” cycle

The paper presents a experimental and mathematical model of interactions between invertebrates (the ciliates Paramecium caudatum and the rotifers Brachionus plicatilis) in the “producer–consumer” aquatic biotic cycle with spatially separated components. The model describes the dynamics of the mixed culture of ciliates and rotifers in the “consumer” component, feeding on the mixed algal culture of the “producer” component. It has been found that metabolites of the algae Scenedesmus produce an adverse effect on the reproduction of the ciliates P. caudatum. Taking into account this effect, the results of investigation of the mathematical model were in qualitative agreement with the experimental results. In the “producer–consumer” biotic cycle it was shown that coexistence is impossible in the mixed culture of invertebrates of the “consumer” component. The ciliates P. caudatum are driven out by the rotifers B. plicatilis.     

Why should the latitude of the observer be considered when modeling gradual proton events? An insight using the concept of cobpoint

The shape of flux profiles of gradual solar energetic particle (SEP) events depends on several not well-understood factors, such as the strength of the associated shock, the relative position of the observer in space with respect to the traveling shock, the existence of a background seed particle population, the interplanetary conditions for particle transport, as well as the particle energy. Here, we focus on two of these factors: the influence of the shock strength and the relative position of the observer. We performed a 3D simulation of the propagation of a coronal/interplanetary CME-driven shock in the framework of ideal MHD modeling. We analyze the passage of this shock by nine spacecraft located at ∼0.4 AU (Mercury’s orbit) and at different longitudes and latitudes. We study the evolution of the plasma conditions in the shock front region magnetically connected to each spacecraft, that is the region of the shock front scanned by the “cobpoint” (Heras et al., 1995), as the shock propagates away from the Sun. Particularly, we discuss the influence of the latitude of the observer on the injection rate of shock-accelerated particles and, hence, on the resulting proton flux profiles to be detected by each spacecraft.     

How do interplanetary shock impact angles control the size of the geoeffective magnetosphere?

In this paper, we investigate temporal and spatial magnetosphere response to the impact of interplanetary (IP) shocks with different inclinations and speeds on the Earth’s magnetosphere. A data set with more than 500 IP shocks is used to identify positive sudden impulse (SI⁺) events as expressed by the SuperMAG partial ring current index. The SI⁺ rise time (RT), defined as the time interval between compression onset and maximum SI⁺ signature, is obtained for each event. We use RT and a model suggested by Takeuchi et al. (2002) to calculate the geoeffective magnetospheric distance (GMD) in the shock propagation direction as a function of shock impact angle and speed for each event. GMD is a generalization of the geoeffective magnetosphere length (GML) suggested by Takeuchi et al. (2002), defined from the subsolar point along the X line toward the tail. We estimate statistical GMD and GML values which are then reported for the first time. We also show that, similarly to well-known results for RT, the highest correlation coefficient for the GMD and impact angle is found for shocks with high speeds and small impact angles, and the faster and more frontal the shock, the smaller the GMD. This result indicates that the magnetospheric response depends heavily on shock impact angle. With these results, we argue that the prediction and forecasting of space weather events, such as those caused by coronal mass ejections, will not be accurately accomplished if the disturbances’ angles of impact are not considered as an important parameter within model and observation scheme capabilities.     

How the astronomical aspects of climate science were settled? On the Milankovitch and Bacsák anniversaries,with lessons for today

It was 100 years ago (on August 7, 1920), that the comprehensive mathematical foundations of climate change research, written by a Serbian researcher, Milutin Milankovitch, were published. A later interpreter and developer of his results, Georg (in Hungarian: György) Bacsák (Pozsony/Pressburg/Bratislava, June 5, 1870 - Fonyód, March 4, 1970) was born 150 years ago and died at the age of one hundred, half a century ago. In this commemorative paper we look back to special circumstances in revealing the secrets of ice ages that had puzzled scientists for at least several centuries. Recently, after 100 years, the Milankovitch theory, including related short-term forcings (ranging from interannual, multidecadal to millennial timescales) has not only been confirmed, but its climate forcing mechanism has also been identified and proposed. Owing to the uniqueness of the problem, the science of the orbital forcing of climate change can be proclaimed to be essentially settled.     

Aerosols and clouds in the upper troposphere–lower stratosphere region detected by GOMOS and ACE: Intercomparison and analysis of the years 2004 and 2005

Satellite-based limb occultation measurements are well suited for the detection and mapping of polar stratospheric clouds (PSCs) and cirrus clouds. PSCs are of fundamental importance for the formation of the Antarctic ozone hole that occurs every year since the early 1980s in Southern Hemisphere spring. Despite progress in the observation, modeling and understanding of PSCs in recent years, there are still important questions which remain to be resolved, e.g. PSC microphysics, composition, formation mechanisms and long-term changes in occurrence. In addition, it has recently become clear that cirrus clouds significantly affect the global energy balance and climate, due to their influence on atmospheric thermal structure.