Features of the solar-type activity of stars with various depths of the convective zone

The levels of chromospheric and coronal activity of the Sun are compared with new vast observations of late-type stars. The solar chromosphere turned to be more powerful than in the main body of stars and the corona is considerably weakened. A wavelet analysis of activity indices and measurement results for the magnetic field of the Sun as a star was performed for several solar cycles. It was obtained that solar activity in the differential rotation differs from phenomena on less massive K stars with cycles and, in contrast to them, the large-scale magnetic field of the Sun is a regulating factor for active processes. These results can be naturally explained with the assumption that the activity of a star with a given mass depends on the depth of the lower base of the convective zone. This seems to require the development of knowledge about the two-level dynamo and a new approach to studying solar-type activity.     

Variability of sunlike stars

Stars with the same temperature, luminosity, chemical composition, and activity as the Sun may be designated “sunlike stars.” The variability of several dozen reasonably sunlike stars has been monitored regularly since 1966 in chromospheric Ca II HK emission, and since 1984 in the visual continuum; larger stellar samples have been observed less comprehensively. Similar solar time series exist. A comparison of solar variability with its stellar analogs indicates that the Sun's current behavior is not unusual among sunlike stars, although the amplitude of the Sun's cyclic variation, measured photometrically, may be smaller than that of its stellar analogs. If the ensemble characteristics of a sample of sunlike stars are representative of the Sun's possible behavior, then such samples may provide insight about states of solar activity, such as Maunder Minima, which have not been observed on the Sun during the contemporary era of space-based measurements. Future progress in solar–stellar research will likely require studies of (1) rigorously selected samples of sunlike field stars, and (2) larger samples from stellar clusters, observed using 4-m class telescopes equipped with multi-object spectrographs and CCD photometers.     

Manifestations of the ray structure of the coronal streamer belt in the form of sharp peaks of the solar wind plasma density in the Earth’s orbit

White corona images are analyzed based on the calibrated data of the LASCO-C2/SOHO instrument (processing level 1) and the solar wind (SW) parameters with hourly and minute resolutions on the Wind spacecraft. The quasistationary events, excluding coronal mass ejections and their manifestations in SW are studied. It has been indicated that the angular dimensions and relative variations in the density of the streamer belt segments remain almost unchanged over the entire distance from the Sun to the Earth’s orbit. In the Earth’s orbit, the ray structure of the belt streamer manifests itself as sharp (with steep fronts lasting several minutes and less) peaks (of several hours in duration) of the solar wind plasma density with maximal values N _max > 10 cm^?3.     

On the chemical composition of the Moon,Jupiter, meteorites and Am stars

If surface anomalies in the composition of the metallic-line A stars (Am stars) are due to a precipitation of planet-like bodies (planetoids) on them, then one should expect a correlation to exist between the overabundance of heavier-than-iron elements on these stars and their “standard” abundances in the solar system (since chondrites provide the “standard” level for these elements). However, an anticorrelation was revealed.Nevertheless, this fact supports the original suggestion on the origin of the metallicism of A stars, and can easily be explained within the author's hypothesis on the formation of the Sun from matter escaping from the proto-Jupiter. During the terminal stages of mass transfer, the matter was strongly depleted in refractories (forming the rocky core of Jupiter). Therefore the composition of the meteorites formed should not coincide with the primary composition of the matter. Thus the Sun's outer layers may also have a distorted composition. The author concludes that it is desirable to revise the “standard” abundances of elements heavier than iron.From a comparison of the surface composition of Am stars with the composition of lunar anorthosites and that of rocks in the upper zones of the Skaergaard intrusion (Greenland), the Am phenomenon may be seen to result from a precipitation of large geochemically differentiated planetoids onto a star. Such planetoids (including the Moon) condense in the cooled envelope of the primary component of a close binary stellar system.     

The nighttime distribution of ozone in the low-latitude mesosphere

The intensity of stars at wavelengths in the Hartley continuum region of ozone has been monitored by the University of Wisconsin stellar photometers aboard the OAO-2 satellite during occultation of the star by the earth's atmosphere. These occultation data have been used to determine the ozone number density profile at the occultation tangent point. The nighttime ozone number density profile has a bulge in its vertical profile with a peak of 1 to 3×10⁸ cm^–3 at approximately 83 km and a minimum near 75 km. The ozone number density at high altitudes varies by as much as a factor of 4, but does not show any clear seasonal variation or nighttime variation. The retrieved ozone number density profiles define a data envelope that is compared with other nighttime observations of the ozone number density profile and also the results of theoretical models.Calculations are also presented that illustrate the difference in retrieving the bulge in the ozone number density profile from stellar and solar occultation data.The National Center for Atmospheric Research is sponsored by the National Science Foundation.     

Hydrodynamics and Thermodynamics of Newtonian Stars

We investigated spherically symmetric solution for nonrelativistic cosmological fluid equations and thermodynamic equation of state for Newtonian stars. It was shown that the assumption of a polytropic equation, , at the center of the star only suffices to integrate the equations explicitly. Our exact solution yields many fruitful results such as stellar stability, spherical oscillation and collapses of stars. Pressure, temperature, and density profiles inside stars were obtained. Central densities, pressures and temperatures of the Newtonian stars such as Sun, Jupiter and Saturn were also calculated. Collapse and expansion mechanism was explained by the heat transfer mechanism inside star. The upper bound value of white dwarf mass obtained by the Newtonian cosmological fluid equations turns out to be comparable to the static limit of Chandrasekhar one. Motion of the Universe was also discussed within the framework of Newtonian mechanics. Our calculation results without considering nuclear reactions inside stars may be applicable to the formation of protostars.     

Spectroscopy of astrophysic al plasmas in the laboratory

Francis Keenan and Steven Rose examine how and why astrophysicists use plasma in the laboratory to mimic accretion processes in stars.     

Extended horizontal branch stars

Astronomers met at Keele University, Staffordshire, in June to discuss how observations of extended horizontal branch stars have changed our view of hot star atmospheres, stellar winds, single and binary star evolution, stellar pulsations and the age estimates for elliptical galaxies. Pierre Maxted reports.     

The solar Na/Ca and S/Ca ratios: A close comparison with carbonaceous chondrites

Solar abundances based on recent laboratory oscillator strengths confirm the relationship between solar matter and carbonaceous chondrites. Within spectroscopic uncertainties (typically±40%) these meteorites contain refractory and volatile elements in solar proportions. Significant improvement of accuracy at present seems restricted to a few abundant elements having reliable quantum-mechanical oscillator strengths, and necessitates strictly differential spectrum analysis. Taking this into account, the solar abundance ratios Na/Ca and S/Ca have been determined to an accuracy of±15%. The results are:Na/Ca= 0.91and S/Ca= 6.8. These volatile/refractory ratios just match type 1 carbonaceous chondrites, but contrast with other types.These and related interstellar abundance features place constraints on the condensation process and a potential heterogeneity of the solar nebula. There is evidence that no drastic pre-solar separation of interstellar gas and grains has occurred, but minor imbalance may be a common mechanism co-determining stellar metal content.     

Seismology of the corona of the Sun

V M Nakariakov and E Verwichte put seismology to work in the study of the solar corona, the hot atmosphere of the Sun.     

Diagnostics of solar wind streams and their sources in the solar corona

The studies are based on the experimental mass sounding of the interplanetary plasma near the Sun at radial distances of R = 4−70 R _S, performed at Pushchino RAO, Russian Academy of Sciences, and on the calculated magnetic fields in the solar corona based on the magnetic field strength and structure measured on the Sun’s surface at J. Wilcox Solar Observatory, United States. The experimental data make it possible to localize the position of the boundary closest to the Sun of the transition transonic region of the solar wind in the near-solar space (R ≈ 10−20 R _S) and to perform an interrelated study of the solar wind structure and its sources, namely, the magnetic field components in the solar corona based on these data. An analysis of the evolution of the flow types in 2000–2007 makes it possible to formulate the physically justified criterion responsible for the time boundaries of different epochs in the solar activity cycle.     

Life, the universe and everything, with GAIA

Great things are expected of the GAIA Observatory, currently expected to launch in 2011. Gerry Gilmore explains how it will provide accurate measurements that will help us understand the formation of the Milky Way and the distribution of dark matter.
The GAIA Observatory, ESA's Cornerstone 6 mission, addresses the origin and evolution of our galaxy, and a host of other scientific challenges. GAIA will provide unprecedented positional and radial velocity measurements with the accuracies needed to produce a stereoscopic and kinematic census of about one billion stars in our galaxy and throughout the Local Group, about 1% of the galactic stellar population. Combined with astrophysical information for each star, provided by on-board multicolour photometry, these data will have the precision and depth necessary to address the three key questions which underlie the GAIA science case: l when did the stars in the Milky Way form? l when and how was the Milky Way assembled? l what is the distribution of dark matter in our galaxy? The accurate stellar data acquired for this purpose will also have an enormous impact on all areas of stellar astrophysics, including luminosity calibrations, structural studies, and the cosmic distance scale. Additional scientific products include detection and orbital classification of tens of thousands of extrasolar planetary systems, a comprehensive survey of objects ranging from huge numbers of minor bodies in our solar system, including near-Earth objects, through galaxies in the nearby universe, to some 500 000 distant quasars. GAIA will also provide several stringent new tests of general relativity and cosmology.     

Solar-Type Stars with the Suppression of Convection at an Early Stage of Evolution

The evolution of a solar-mass star before and on the main sequence is analyzed in light of the diminished efficiency of convection in the first 500 Myr. A numerical simulation has been performed with the CESAM2k code. It is shown that the suppression of convection in the early stages of evolution leads to a somewhat higher lithium content than that predicted by the classical solar model. In addition, the star’s effective temperature decreases. Ignoring this phenomenon may lead to errors in age and mass determinations for young stars (before the main sequence) from standard evolutionary tracks in the temperature–luminosity diagram. At a later stage of evolution, after 500 Myr, the efficiency of convection tends to the solar value. At this stage, the star’s inner structure becomes classical; it does not depend on the previous history. On the contrary, the photospheric lithium abundance contains information about the star’s past. In other words, there may exist main-sequence solar-mass stars of the same age (above 500 Myr), radius, and luminosity, yet with different photospheric lithium contents. The main results of this work add considerably to the popular method for determining the age of solar-type stars from lithium abundances.

     

Exoplanets

George Cole reviews the properties and significance of the planetary systems discovered around stars other than our Sun.
There has been speculation for centuries that planets might exist around stars other than our Sun. Might they form planetary systems like our solar system? Will life be found elsewhere one day? Planets were, in fact, discovered orbiting a pulsar in 1991 but, more interestingly, companions were found to stars like our Sun four years later. More stars with companions are continually being discovered and some 50 systems are known at the present time. Can some of these orbiting bodies be planets and what might they be made of? Is there a pattern in the systems being found? How do they compare with the solar system? Can they sustain living material? This article attempts to throw light on these questions.     

An annual and a semiannual variation of the upper air density

Summary The fluctuation of the acceleration are analysed for several satellites. For the density variations three predominant influences can be distinguished: 1) The varying solar short ultra-violet radiation; 2) The day-night-effect; 3) An annual variation. The latter suggests a significant interaction of the terrestrial upper atmosphere with the interplanetary matter. The annual variation gives some evidence for an interstellar wind due to the solar motion in the local stellar system.     

Space research of the Sun: Current state and prospects

This paper is a review of the current state and prospects of space research into the Sun, which plays an important role in solar-terrestrial physics studies. We present the most significant results obtained by spacecraft for different fields of solar physics-from the interior to the corona. Goals and tasks of solar space projects under development or consideration are briefly discussed.     

Solar infrared spectral observations around the 1999 solar eclipse

An experiment was performed at the Roseland Community Observatory, Cornwall, during the 11 August 1999 total solar eclipse. The main objective was to search for strong infrared coronal lines with a view to identifying candidates for subsequent coronal magnetic field measurements. In particular we hoped to measure the intensity of the Si IX line at 3.93 m, the most likely candidate line. The secondary aim of the experiment was to search for Rydberg transitions of neutral hydrogen and helium in the corona, previous observations of the infrared corona having produced evidence that cool, in coronal terms, material may co-exist in the corona with the hot (10⁶ K) plasma. The experiment did not succeed in the above aims as the Sun was obscured by cloud on the morning of the eclipse at the Roseland Observatory site. However, infrared observations of the sunlight scattered through the clouds produced a remarkable result. The infrared intensity fell precipitously 6.5 minutes before second contact and rose just as suddenly 6.5 minutes after third contact. The authors are unable to explain this result but suggest that it might be a terrestrial atmospheric rather than a solar phenomenon.
Intriguing observations from the total solar eclipse in Cornwall last year are reported by A Ridgeley, B Sheen, G Barnard, C Corrigan, G E Derbyshire, R Jones, P Moir-Riches, C Purchase, P D Read and T Richards.     

Streamer belt in the solar corona and the Earth’s orbit

It has been indicated that the cross section of the streamer belt in the solar corona and its extension in the heliosphere—heliospheric plasma sheet (HPS)—have the form of two radially oriented closely located (at a distance of d ≈ 2.0–2.5° in the heliocentric coordinate system) rays with increased and generally different densities. The angular dimensions of the rays are ≈d. The neutral line of the magnetic field in the corona and the related sector boundary in the Earth’s orbit are located between the peaks of densities of these two rays. In the events, during which the true sector boundary coincides with the heliospheric current sheet, the transverse structure of the streamer belt in the heliosphere (or the HPS structure) is quasistationary; i.e., this structure slightly changes when the solar wind moves from the Sun to the Earth in, at least, 50% of cases. A hypothesis that a slow solar wind, flowing in the rays with increased density of the streamer belt, is probably generated on the Sun’s surface rather than at the top of the helmet, as was assumed in [Wang et al., 2000], is put forward.     

Global Oscillations of the Sun according to SOHO/LASCO C3 Coronagraph Data

Geomagnetism and Aeronomy - Long-period oscillations in the brightness of the Sun as a star have been analyzed on the basis of measurements of the solar light reflected by planets when they come...     

Radiation belt storm probes: Resolving fundamental physics with practical consequences

The fundamental processes that energize, transport, and cause the loss of charged particles operate throughout the universe at locations as diverse as magnetized planets, the solar wind, our Sun, and other stars. The same processes operate within our immediate environment, the Earth's radiation belts. The Radiation Belt Storm Probes (RBSP) mission will provide coordinated two-spacecraft observations to obtain understanding of these fundamental processes controlling the dynamic variability of the near-Earth radiation environment. In this paper we discuss some of the profound mysteries of the radiation belt physics that will be addressed by RBSP and briefly describe the mission and its goals.