Based on analyzing the fine structure of time series of solar and heliospheric parameters a universal numerical technique is developed to study large-scale patterns of solar activity and the heliospheric structure. The Solar Mean Magnetic Field (SMMF) time series and the magnetic fields in solar corona (Hoeksema & Scherrer 2004) were studied in time-longitude aspect (figures 1a,b,c,d). It is shown that the behavior of the large-scale magnetic field, its multiperiodic rotation determine the heliospheric structure and changes in space weather (Mordvinov & Plyusnina 2004). Time-longitude analysis of Interplanetary Magnetic Field (IMF) near the Earth (King et al. 2004) reveals similar diagram (figure 1e) shifted relative to the photospheric and coronal magnetic fields by the transport time.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

A new information resource to study solar magnetic field variations and their influence on the Earth extending ordinary lengths of some traditional indices of solar activity is introduced.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We discuss the results so far of a program to image in the rest-frame optical and near-UV the host galaxies of a sample of 5 high redshift (z∼2−3) radio-quiet quasars with nuclear luminosities lower than most samples studied at high z. We found that in the rest-frame optical the hosts have luminosities of about L∗, comparable to the Lyman break galaxies at similar redshifts. From the rest-frame UV imaging, we can derive optical–UV colors, and find they show a great deal of variation, but may be somewhat redder and less starforming than the LBGs. We are supplementing this work at high z with study of the hosts of z∼1 radio-quiet quasars with similar low nuclear luminosities.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The short-term periodicities of the flare index (FI) which is roughly proportional to the total energy emitted by the flare, are investigated in detail using Fourier transform (FT) for the full-disc and for the northern and the southern hemispheres of the Sun separately over the epoch of almost 4 cycles (1966-2002) which covers 13392 days. Figure 1 shows the power spectra of the three time series of FI calculated for the 289-771 nHz (15-40 days) range with 0.24 nHz interval. The uncertainty in each frequency is ±0.4 nHz due to the 36.5-year data length. The dashed lines indicate the false alarm probability significance levels. In this figure, there are several pronounced power peaks whose significances are enough high. These are at 25.6, 27.0, 30.2 days for the full-disc, 27.0 days for the northern hemisphere and 27.5 and 33.8 days for the southern hemisphere. Since commonly used FT is not able to disclose the possible changes in the periodicities over the period studied, the wavelet transform (WT) was applied to search for temporal variability. The wavelet transform results show that the occurence of periodicities of flare index power is highly intermittent in time. All three FI time series show that the major periods, obtained by Fourier transform are localised in short time intervals (typically up to half of a year).To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present VLT–ISAAC spectra of unprecedented S/N and resolution for the Hβ region in a sample of n = 17 quasars in the range z=0.8–2.5. The data represent our first attempt to test source occupation and line properties for the Eigenvector 1 parameter space that was defined using a sample of sources with z<0.8. We find no strong luminosity/redshift dependent effects with the possible exception of an increase in the minimum broad line profile width from 1000 to 3000 km s−1 between MB≈−20 and −28.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The cause of 92 geomagnetic disturbances in the period of 1997 – 2003 was analyzed. There were used data from LASCO C3 instrument from SOHO satellite, SOHO LASCO CME Catatalog, and the daily average indices Ap. In this contribution we proposed to search sources of the geomagnetic storms taking into account the old idea by Newkirk and Bohlin (1965). According to this idea a solar coronal streamer can cause geomagnetic disturbance when it crosses the Earth's space.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Based on our previous work about a co-evolution of massive black holes (MBH) and their host spheroids, we estimate the cosmic star formation history associated with AGN accretion by ROSAT X-ray All sky surveys. We show: 1) the total amount of star formation associated with MBH growth is at least half of the net star formation at high redshift, which probably totally missed by the current UV/optical deep surveys; 2) the FIR emission from the dust heated by star formation on-going during the MBH growth could be a significant energy source for SCUBA populations; 3)the peak redshift of the massive spheroid formation in this case is around 1.5, not necessary to be at much higher redshift.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The investigation of coronal holes (CH) is in progress now thanks to a number of high precise experimental projects and a lot of observations (Ulysses, SOHO, Yohkoh and many others). Historical epoch of CH discovery and study is prolonged today on the new experimental materials. Our considerations of CH and its manifestations in SW near the Earth were connected with minimum, growth and maximum phases of solar cycle. In this work we deal with the descending phase of solar cycle 23. There was the interval of comparatively quite Sun in March 2004, when strong sporadic phenomena were not observed. The existence of long-lived transequatorial recurrent coronal holes on the solar disk allows the investigation it imprinting in SW flows, using Wind data in near Earth cosmic space, data SOHO, Yohkoh and others.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

In order to analyse the large numbers of Seyfert galaxy spectra available at present, we are testing new techniques to derive their physical parameters fastly and accurately.

We present an experiment on such a new technique to segregate old and young stellar populations in galactic spectra using machine learning methods. We used an ensemble of classifiers, each classifier in the ensemble specializes in young or old populations and was trained with locally weighted regression and tested using ten-fold cross-validation. Since the relevant information concentrates in certain regions of the spectra we used the method of sequential floating backward selection offline for feature selection.

Very interestingly, the application to Seyfert galaxies proved that this technique is very insensitive to the dilution by the Active Galactic Nucleus (AGN) continuum. Comparing with exhaustive search we concluded that both methods are similar in terms of accuracy but the machine learning method is faster by about two orders of magnitude.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Here we show that archaeomagnetic measurement confidence interval ($\alpha_{95}$) may serve as a new proxy for the past solar activity estimation. This proxy is compared with sunspot numbers during 1700-2000 yr and with other proxies during 1500–2000 yr.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Abundances in Galactic globular clusters are important for understanding Galactic chemical evolution and the formation of the Milk Way. 47 Tucanae (NGC 104) is a template metal-rich globular cluster ([Fe/H] ∼–0.7 dex). From the point of view of high resolution spectroscopy, there is still a lack of abundance analyses in the literature. In this work we present a detailed analysis carried out for 5 giants stars (12.10 < V < 14.30) of 47 Tucanae, using high resolution spectra (λ/Δλ∼60,000) with high signal-to-noise ratio (S/N > 200), obtained at the ESO VLT-UT2 8m telescope, equipped with the UVES spectrograph. Abundances of α- (O, Mg, Ca, Si, Ti), s- (Ba, Y, Sr) and r- (Eu) process elements are obtained.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We have used most recent archaeomagnetic and ice core $CO_2$ records for the long-term trend correction in global tree ring radiocarbon concentration ($\Delta^{14}C$). The short-term $CO_2$ exchange system was approximated via first order differential equation with frequency dependent coefficients. A generalized multi-scale box model was constructed and used for the reservoir effect correction.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present here the self-similar collapse of a relativistic singular isothermal sphere (SIS) that leads to monolithic black hole formation. The dynamic evolution is triggered by the central portion of the SIS collapsing to for an infinitesimal black hole. This perturbation removes the pressure support for the layer immediately above, which causes it to collapse, and so on. The influence of gravitational collapse propagates out as an expansion wave moving at the speed of sound. Outside of the expansion wave, matter remains in local equilibrium.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present a brief review of published results on the geomagnetic storm effectiveness of CMEs and solar flares as well as of interplanetary events. Attention is drawn to the fact that the published values of storm effectiveness are in conflict with one another. Possible reasons of their differences are discussed.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The “Herschel Space Observatory” is an ESA mission to perform imaging photometry and spectroscopy in the far-IR & submm 57–670 μm range. It carries a 3.5 m diameter radiatively cooled telescope. The scientific instruments – two cameras/medium resolution spectrometers (PACS and SPIRE) and a very high resolution heterodyne spectrometer (HIFI) – are housed in a superfluid helium cryostat. Herschel will be placed in orbit around the Earth-Sun L2 point in 2007 and will operate for a minimum of 3 years. Roughly 2/3 of the observing time is open to the general astronomical community through a competitive proposal procedure.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The very weak storm-effectiveness of frontside partial halo coronal mass ejections (FPH CMEs) suggests that many, if not most, FPH CMEs are not Earth-directed. Based on the cone model (Zhao et al., 2002) we put forward a method to identify Earth-directed partial halo CMEs from FPH CMEs.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We predict the metallicity distribution of stars for 6 Dwarf Spheroidal (dSph) galaxies of the Local Group by means of a chemical evolution model which is able to reproduce several observed abundance ratios and the present day total mass and gas content of these galaxies. The model adopts up to date nucleosynthesis and takes into account the role played by supernovae of different types (II, Ia). Each galaxy model is specified by the prescriptions of the star formation rate and by the galactic wind efficiency chosen to reproduce the main features of these galaxies.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

A single web link is provided to a maintained site giving detailed descriptions of telescope and instrumentation combinations available – and planned for the near future – at Gemini South, CTIO, SOAR and SMARTS for observers of AGN.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present a brief review of scientific milestones of the Russian Space Research Program for 2006-2015 in the field of solar and solar-terrestrial physics and describe several space projects: CORONAS-PHOTON, RESONANCE, CLIPPER, INTERHELIOPROBE, and THERION-F2.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The Advanced Technology Solar Telescope (ATST) will perform high-resolution studies of the Sun's magnetic fields needed to understand their role in the fundamental processes responsible for solar variability. The generation of magnetic fields through dynamo processes, the amplification of fields through the interaction with plasma flows, and the destruction of fields remain poorly understood. There is incomplete insight as to what physical mechanisms are responsible for heating the corona, what causes variations in the radiative output of the Sun, and what mechanisms trigger flares and coronal mass ejections. Progress in answering these critical questions requires study of the interaction of the magnetic field and convection with a resolution sufficient to observe scales fundamental to these processes.

The 4-m aperture ATST is designed as a unique scientific tool, with excellent angular resolution, a large wavelength range, and low scattered light. With its integrated adaptive optics, the ATST will achieve a spatial resolution nearly 10 times better than any existing solar telescope.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html