To explain the origin of hard X-ray emission, we suggest the internal shocks could be created in the reconnection jet and accelerate the energetic particles in the solar flares. We examine its possibility by performing 2D resistive MHD simulations. We use very small very small grid to resolve the diffusion region and remove the effect of numerical noise. As the results, the current sheet becomes thin by tearing instability, and collapses to Sweet-Parker sheet. It becomes unstable again so that the secondary teaing instability occurs. Immediately after the plasmoid ejection, anomalous resistivity sets in and Petschek-like reconnection starts. During the Petschek reconnection, many plasmoids are created by the secondary tearing instability and ejected along the current sheet. The multiple fast shocks are created in the current sheet. We suggest that the internal shocks shown in this paper are possible sites for the particle acceleration in the solar flares.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Our view of galaxy evolution has been dramatically enhanced by recent deep field surveys at far-infrared and submillimeter wavelengths. Current evidence suggests that the number density of the most luminous far-infrared sources evolves strongly with redshift, and that the luminosity density in the far-infrared/submillimeter may exceed that in the optical/ultraviolet by factors of 3−10 at redshifts z > 1. If true, then as much as 80-90% of the “activity” in galaxies at z > 1 may be hidden by dust. Surveys of complete samples of luminous infrared galaxies in the local Universe show that the majority, if not all objects with log $(L_{\rm ir}/L_\odot) \simgt 11.6$, appear to be major mergers of molecular gas-rich disks accompanied by dust-enshrouded nuclear starbursts and powerful AGN. If the majority of the deep-field sources are simply more distant analogs of local luminous infrared galaxies, then we may be witnessing at z ∼1−3 the primary epoch in the formation of spheroids and massive black holes. This major event in galaxy evolution is largely missed by current deep optical/ultraviolet surveys.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

TRACE (Transition Region and Coronal Explorer) observations of transverse oscillations in coronal loops have prompted a number of questions to which there are no convincing answers as yet. Only the conclusion that the appearance of oscillations reflects the response of the magnetosphere of an active region to an internal or external magnetohydrodynamic (MHD) disturbance seems beyond question. The sources of such disturbances are solar flares or filament eruptions. The putative correspondence of the observed oscillations to the axisymmetric fundamental kink mode of a single coronal loop raises two questions at once: how to excite this mode and how to explain the rapid damping of the oscillation.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We discuss obbservations and numerical simulations which show that radiative shocks in jet-cloud collisions can trigger the collapse of intergalactic clouds and subsequent star formation in low luminosity, ‘FR-I’ type, radio galaxies.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

XSM is a calibration subinstrument of D-CIXS onboard the SMART-1 technology mission to the Moon. SMART-1 was launched in September 2003 from Kourou, French Guyana, and the instruments onboard are now scientifically operational at the time of writing. XSM provides a 52 degree field of view in the energy range of 1-20keV. We have cross calibrated XSM with GOES, and the fidelity of XSM data seems highly likely.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

This work is devoted to the new phenomena appearing in radio emission in preflare active regions that were found with the use of radio telescope RATAN-600. The first is the complicated spectral-polarization behavior in narrow frequency range and, in particularly, the double changing of the polarization emission sign in active region at the time interval of several days before big flare. The second, the detection of regular decreasing of radio brightness radio darkening of active regions, which is also observed in a few days prior to flare [Tokhchukova & Bogod (2003)].To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We discuss some recent results from a program to study the relationships between AGNs, super-massive black holes (SMBHs), and their surrounding host galaxies. The results are based on broad emission-line diagnostics of the SMBH masses and metal abundances in a unique sample of 578 Type 1 AGNs.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

An aestimate of a typical life time of zebra pattern associated with escaping of fast particles from the trap into the loss-cone, is given. Besides, we estimate a number of fast electrons that is necessary to be injected into the trap in order to provide the observed brightness temperature of zebra stripes.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The formation and growth of supermassive black holes (SMBHs) physically linked with bulges are considered. We focus on the radiation hydrodynamic process for the growth of SMBH in the optically thick starburst phase, where radiation from bulge stars drives the mass accretion on to a galactic center through radiation drag effect. In the present scenario, the AGN luminosity-dominant phase (QSO phase) is preceded by the host luminosity-dominat phase, which is called “proto-QSO phase”. In this phase, there exists the massive dusty disks within younger bulges. Also, the proto-QSO phase is anticipated by an optically-thick ultraluminous infrared galaxy (ULIRG) phase. Furthermore, such radiation hydrodynamic model has been also applied to disk galaxies. It turns out that the mass of a SMBH primarily correlates with a bulge component even in a disk galaxy. Thus, by analogy to proto-QSOs, the BH growing phase in disk galaxies may have massive dusty disks within younger bulges.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present near-infrared imaging of the host galaxies of 17 quasars at 1 < z < 2, obtained with ISAAC at the ESO VLT UT1 under excellent seeing (∼0.4 arcsec). The radio-loud (RLQ) and radio-quiet (RQQ) quasars in the sample have similar distribution of redshift and optical luminosity. Both RLQ and RQQ hosts follow the cosmic evolution of massive inactive ellipticals undergoing passive evolution. This indicates that nuclear activity can occur in all luminous ellipticals without producing a significant change in their global properties and evolution. However, there is a systematic difference by a factor ∼2 in the host luminosity between RLQs and RQQs, which remains the same from z = 2 to z = 0. Quasar hosts are already well formed at z ∼2, in disagreement with hierarchical models of AGN and galaxy formation and evolution models. No correlation is found between the nuclear and the host luminosities. If the host luminosity is proportional to the black hole mass, as in nearby massive spheroids, both types of quasars emit at very different levels with respect to their Eddington luminosity.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The one-dimensional relaxation of a spatially bounded electron stream in non-uniform background plasma is simulated. The corresponding system of quasi-linear equations is \begin{equation}\frac{\partial f}{\partial t}+V\frac{\partial f}{\partial x}=\frac \partial {\partial V}\left( D\frac{\partial f}{\partial V}\right),\, \frac{\partial W}{\partial t}=2\gamma W,\, \gamma =\frac \pi 2\frac{\omega _p}{n_p}V^2\frac{\partial f}{\partial V},\, D=\frac{8\pi ^2e^2}{m^2}\frac WV. \end{equation} Here $f$ - the electron distribution function, $D$ - diffusion coefficient, and $\gamma$ and $W$ - are the growth rate and spectral energy density of plasma waves respectively, $n$ - background plasma density, $\omega_p$ - plasma frequency. Initial conditions (the electron distribution function at $t = 0$): \begin{equation}f(x,V,t=0)=An_{b}\exp \left(-\frac{(V-V_b)^2}{2V_{Tb}^2}\right)\exp \left(-\left(\frac xd\right)^2\right)\end{equation}To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Coronal mass ejections (CMEs) are a key aspect of coronal and interplanetary dynamics. They can inject large amounts of mass and magnetic fields into the heliosphere, causing major geomagnetic storms and interplanetary shocks, a key source of solar energetic particles. Studies over the past decade using the excellent data sets from the SOHO, TRACE, Wind, ACE and other spacecraft and ground-based instruments have improved our knowledge of the origins and early development of CMEs at the Sun and how they affect space weather at Earth. I review some key coronal properties of CMEs, their source regions, their manifestations in the solar wind, and their geoeffectiveness. Halo-like CMEs are of special interest for space weather because they suggest the launch of a geoeffective disturbance toward Earth. However, their correspondence to geomagnetic storms varies over the solar cycle. Although CMEs are involved with the largest storms at all phases of the cycle, recurrent features such as interaction regions and high speed wind streams can also be geoeffective. A new heliospheric experiment, the Solar Mass Ejection Imager, has completed its first year in orbit and I give some early results.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present the black hole mass–bulge velocity dispersion relation for a complete sample of 75 soft X-ray selected AGNs. We find that the AGNs with highest accretion rates relative to Eddington lie below the MBH–σ relation of broad line Seyfert 1s, confirming the Mathur et al. (2001) result. The statistical result is robust and not due to any systematic measurement error. This has important consequences towards our understanding of black hole formation and growth: black holes grow by accretion in well formed bulges. As they grow, they get closer to the MBH–σ relation for normal galaxies. The accretion is highest in the beginning and dwindles as time goes by. Our result does not support theories of the MBH–σ relation in which the black hole mass is a constant fraction of the bulge mass/velocity dispersion at all times or those in which bulge growth is controlled by AGN feedback.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We briefly review several aspects of the quasi-stationary structure of the corona in relation with the helio-sheet and, also, of the more confined by the magnetic field structures, including streamers, loops, jets, plumes and narrow linear rays. Both the temperature and the density structures are tentatively considered. Flows deduced from proper motions analysis are discussed. We did not include CMEs and flares in this presentation but other more radial and possibly highly impulsive beams with flows are discussed. We stress the importance of the variations of the coronal magnetic field and inferred currents in explaining the observed structures.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

In this work I present the survey which is searching for the rise in the volume-averaged star formation rate at intermediate redshifts (z<1). This survey is a combination of the data taken with Advanced Camera for Surveys in parallel with WFPC2 (U band) of the GOODS fields. We use template fitting of the spectral energy distributions to obtain photometric redshifts and classify the objects as starbursts, early- and late-types. The colors of the starbursts were reproduced and ages were estimated with the stellar evolutionary synthesis code Starburst99. By matching the optical catalog with the Chandra X-ray catalog we have identified the X-ray sources and possible candidates for having a combination of active nuclei and starburst at intermediate redshifts. Analysis of the light concentration, asymmetry and clumpiness, shows that this sample is a mixed bag, containing dwarf ellipticals, early and late-spirals and peculiar objects which resemble mergers in progress. These results have strong implications for galaxy evolution since it shows for the first time who are the candidates for the rise of the SFR at intermediate-z.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Available YOHKON, TRACE, SOHO/EIT and CORONAS-F data are interpreted as evidences of the non-local coronal mass ejection initiation processes when rapidly increasing electric currents appear in the coronal loops and arcades. These electric currents are driven by subphotospheric processes. Self-similar plasma motions are due to the electric drifts in crossed inductive electric and magnetic fields. Expanding non-planar loops often mimic “reconnection” features, being in reality projection effects of the “twist and fold” processes on the image plane. Among such patterns one can find examples of spurious x-points, concave fronts, blobs, islands, etc. Coronal mass ejections often proceed without large scale topological changes of magnetic fields. They are accompanied by enhanced small-scale turbulence.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present HST/STIS FUV images of the Lyα and FUV continuum emission of the luminous emission line nebulae in the cooling core cluster A1795. The Lyα and FUV continuum emission consist of a diffuse component (∼60%) and more compact features (knots and filaments) which lie preferentially along the radio source edges. The correlations between the FUV continuum flux and the Lyα emission line flux implies that the nebulae are mainly ionized locally. We suggest that the FUV knots are star clusters with ongoing star formation with rates of several solar masses per year. It appears that star formation occurs through out the nebula, though it is strongly enhanced along the edges of the radio source. The radio source may play a key role in the ionization and morphology of the nebula, e.g., by snow-plowing the gas, shocking and ionizing the gas, triggering star formation, and destroying clouds that it has engulfed. The observed FUV continuum is consistent with about half the number of hot stars which are required to ionize the nebula. We note that we may be missing some of the FUV flux due to obscuration. Thus, we find that young hot stars (e.g., O5) probably provide the bulk of the photons which ionize the nebula, though other sources of ionization may contribute in selected regions of the nebula. We suggest that the mass accretion rates are comparable to the star formation rates (of order 10 M[odot ] yr−1). This is consistent with the lack of intermediate temperature gas (<1 keV) being due to energy input to the cooling gas, rather than to “hiding” the cooling gas.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Recent detection of a large optical depth to Thomson scattering by Wilkinson Microwave Anisotropy Probe (WMAP) implicates in new considerations about reionization epoch. Nowadays it is possible to simulate hydrogen reionization for redshift 15 < z < 20, although the greater difficult problem consists to know what are the first ionizing sources in the universe. Observations on Gunn-Peterson effect reconciled with WMAP findings suggests z ∼6 as the redshift for complete reionization. Study on the formation history of supermassive black holes (SMBHs) in galaxies suggests an interplay among QSOs activity and star rate formation. On this aspect, QSOs work as clocks of star formation in spheroids. Observations of magnesium abundance in QSOs for various redshifts show that star formation in these systems began very early.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We provide a brief overview of properties of transequatorial loops (TLs) and show that some TLs fit the description of a loop, while others appear to be the magnetic separators.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We discuss the discovery of six bright Lyman break galaxy candidates in the Sloan Digital Sky Survey and the follow-up observations necessary to determine whether they are powered by star formation or by active galactic nuclei.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html