We examine the energetics of the best examples of flux-rope CMEs observed by LASCO in 1996-2001. We find that 69% of the CMEs in our sample experience a driving power in the LASCO field of view. For these CMEs which are driven, we examine if they might be deriving most of their driving energy by coupling to the solar wind. We do not find conclusive evidence to support this hypothesis. We adopt two different methods to estimate the energy that can possibly be released by the internal magnetic fields of the CMEs. We find that the internal magnetic fields are a viable source of driving power for these CMEs.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

In stars with sufficiently small projected rotational velocities (less than a few ${\rm km\,s}^{-1}$), it is often possible to detect signatures of the atmospheric velocity field in line profiles. These signatures may be as subtle as small asymmetries in the profile (“line bisector curvature”) or as obvious as profile shapes that strongly depart from those predicted by simple microturbulence models. We have recently carried out a high resolution survey of sharp-line stars to search for these symptoms of local velocity fields. We report the first results of a comparison of models with the observed profiles.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

High resolution B, V, I imaging of the inner region of the spiral barred galaxy NGC 7479 suggests this galaxy contains a pseudo nuclear ring and possibly a nuclear bar.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Signs of quasi-regular structures in time-averaged photospheric images are described.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

After a brief overview of solar energetic particle (SEP) emission from coronal mass ejection (CME) shocks, we turn to a discussion of their transport and acceleration. The high energy SEP are accelerated near the Sun, and because of their well-known source location, their transport can be modeled quantitatively to obtain precise information on the injection function (number of particles emitted vs. time), including a determination of the onset time to within 1 min. For certain events, transport modeling also indicates magnetic topology with mirroring or closed field loops. Important progress has also been made on the transport of low energy SEP from very strong events, which can display exhibit interesting saturation effects and compositional variations. The acceleration of SEP by CME-driven shocks in the interplanetary medium is attributed to diffusive shock acceleration, but the spectrum of SEP production is typically modeled empirically. Recent progress has largely focused on using detailed composition measurements to determine fractionation effects of shock acceleration and even to clarify the nature of the seed population. In particular, there are many indications that the seed population is suprathermal (pre-energized) and the injection problem is not relevant to acceleration at interplanetary CME-driven shocks. We argue that the finite time available for shock acceleration provides the best explanation of the high-energy rollover.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present results of stratification analyses for Mg, Si, Ca, Cr and Fe in the atmospheres of two Cr-type sharp-lined peculiar stars HD 133792 and HD 204411. Even in the absence of strong magnetic fields their atmospheres are stable which is confirmed by zero microturbulence. Both stars are slightly evolved, their $\log g \approx 3.5$, whereas their effective temperatures are 9200 and 8400 K, respectively. We find a moderate Cr and Fe stratification. However the abundances of these elements do not fall below the solar value throughout the atmosphere. Si and Ca are strongly stratified, in particular in HD 133792, with large underabundances in the outer atmospheric layers. Abundance stratifications derived for weakly magnetic Ap stars are compared with the empirically determined stratification in the atmospheres of strongly magnetic Ap stars in the same temperature range.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

A main topic at this meeting is how galaxies are affected when they enter for the first time the cluster environment from the outskirts. Most of the times we are forced to infer the environmental effects indirectly, relying on systematic variations of galaxy properties with environment, but there aren't many examples of direct observations able to unveil ongoing transformations, and the corresponding mechanism producing it. We present a case in which it is possible to identify the cluster environment, and in particular the intracluster medium and the recent infall history of galaxies onto the cluster, as the cause for a recent, abrupt change in the evolutionary history of galaxies.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present and discuss results concerning a study of stellar populations in the galaxies belonging to CL 0048-2942, a cluster at intermediate redshift (z = 0.64), and to the field. This study gives insight on the evolutionary stage of the cluster galaxies at different radial distances from the cluster centre. We find a population gradient within the cluster: centre galaxies host older stars whereas galaxies located towards the cluster outskirts are predominantly made of less evolved stars. This effect is even more pronounced as we move outside the cluster, into the field. This is interpreted as star formation being more intense in the field, or rather, suppressed within the cluster, particulary as we move towards its centre.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Very large solar energetic particle (SEP) events occur at the rate of about 10 per year during solar maximum. The primary accelerators in these events are shocks driven by fast coronal mass ejections, in which speeds are greater than about 1000 km/s. Solar Cycle 23 probably produced the largest fluence of > 10 MeV/nucleon SEPs seen since the start of the Space Age. New instruments on Wind, ACE, SOHO, and other satellites have provided unprecedented detail on the energy spectra, elemental and isotopic composition, ionic charge states, and temporal evolution of these SEP events, as well as their associated CMEs and flares. In this talk, I will review some of the new insights provided by these data. A particular challenge in SEP studies has been the very large event-to-event variability in composition and spectral characteristics, particularly at energies above a few tens of MeV per nucleon. I will discuss recent efforts to understand this variability in terms of seed populations and shock geometry. I will also review recent studies of the time at which SEPs first appear on the Sun-Earth magnetic field line and the implications of these studies for the conditions under which SEP production was initiated.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Torsional oscillations of sunspots were investigated in a penumbra on the observations in the photosphere of the longitudinal magnetic and velocity fields.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The XMM–LSS project is detecting distant clusters of low mass, quite comparable in mass to the ones in the local universe. This allows a direct comparison of galaxy properties at different redshifts in “similar” clusters. We present here first results on the evolution of the reddest galaxies in 25 clusters/groups at $0.3\la z \la 1.0$ and for the whole galaxy population in the same clusters. The emerging picture from the current study is that the counterparts of present day clusters tend to show two or more distinct populations: a relatively old ($z_f \gt 2-5$) population evolving passively, together with a younger population, ostensibly responsible for the apparent brightening of the characteristic magnitudes, $m^*$.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

By means of 2D spectroscopy we have found a lot of compact inner stellar and gaseous disks in morphologically normal galaxies. The evolution and spatial orientation of these inner structures are often decoupled from the evolution and spatial orientation of the large-scale galactic disks and bulges. We argue that this finding requires substantial change of common approaches to investigations of the central parts of galaxies, including central black hole studies.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

A new parametric method that approximates the radiative accelerations of bound-bound and bound-free transitions at large optical depths is presented. The parameters found in these new equations are calculated for the following trace elements: C, N, O, Ne, Na, Mg, Al, Si, S, Ar, Ca, and Fe and are made available to potential users. This method can be easily implemented in existing codes to study atomic diffusion without needing large computing resources or access to large atomic and opacity data bases.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

In September 2002 the discovery of a super Li-rich F-dwarf (J 37) in NGC 6633, an iron poor analogue of the better studied Hyades and Praecepe open clusters, was announced. This unique star was thought to be the smoking gun for the action of diffusion, models of which predict a narrow “Li-peak” at approximately the correct temperature. However, with more detailed studies into J 37's abundance pattern this star provides firm evidence for the accretion of planetesimals or other material from the circumstellar environment of new born stars.

Thanks to the specific predictions made about the behaviour of Be abundances, (the most striking of which being no Be in super-Li-rich dwarfs subject to diffusion) the opposing diffusion/accretion predictions can be tested.

Initial modelling of the Be line indicates that J 37 is as Be rich as it is Li rich; $\log N({\rm Be}) = 2.25 \pm 0.25$, and so is broadly consistent with an accretion-fuelled enhancement. However, that both Li and Be are enhanced by much more than the iron-peak elements (as determined in previous studies) suggests that diffusion also plays a role in increasing the abundances of Li and Be specifically.

Furthermore, a new data set from the UVES/UT2 combination has allowed the elemental abundance of iron to be measured. The preliminary stellar parameters are; $T_{\rm eff} \sim 7340\,{\rm K},\log g \sim 4.1$, microturbulence $\sim 4.3 {\rm km s^{-1}}, [{\rm Fe}/{\rm H}] \sim 0.50$. This again provides distinct evidence for the effects of accretion in J 37 and requires a new synthesis of the Be doublet.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The solar active region No. 10486 can be considered as one of the very large and powerful active regions since 1976. This region has produced the most important two solar flares during the period (1976-2003). The first flare released at 12:15UT on 28 October 2003 with importance X17/4B, and the second flare released at 22:25UT on 4 November 2003 with importance X28/3B. Both flares are the highest level in x-ray production since 1976, when different detectors, onboard various spacecrafts, have taken the data, and since 1996, when SOHO was launched to space. The first flare on 28 October 2003 produced protons events at 6:15UT on 29 Oct. 2003 with energies > 10 MeV. The maximum solar wind speed is 1905 and 1986 km/sec at 29 and 30 October 2003 respectively. The same region after its rotation across the sun was appeared again on the sun's edge at 18 November 2003, and produced high energetic flare at 19 November 2003, which led to increase the solar wind speed to 947 km/sec at 20 November 2003. The evaluation of the active region No. 10486 is very important for understanding the high energetic proton flares. The aim of this study is to follow the morphological and magnetic changes of the active region before, during, and after the high energetic flares were produced. Also, applying the cumulative summation curves method for the different index of the active region to predict the flare of high energy has been carried out. The results are promising and can be used for proton flares and Geomagnetic storms prediction, few days before their occurrence.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Gradual solar energetic particle (SEP) events are now believed to be associated with CME-driven shocks. As the shock propagates out from the Sun, particles are accelerated diffusively at the shock front and some will escape upstream and downstream into the interplanetary medium. This is in contrast with “impulsive” events, which are believed to be due to solar flares. However, recent observations have found that in some gradual SEP events, the time intensity profile show a two peak feature, suggesting a mixture of particles from solar flares with particles from CME-driven shock. Furthermore, the observed spectra of large SEP events show tremendous variability. The $Fe/C$ ($Fe/O$) ratio behave oppositely in events which have similar solar progenitors. In this work, we use a numerical model to follow particle acceleration and transport at CME-driven shocks. We investigate a possible scenario for the re-acceleration of flare particles by CME-driven shocks and calculate the $Fe/O$ ratio for two exemple shocks. These simulations are helpful in interpreting observations of particle data obtained in situ at 1 AU by spacecraft such as ACE and WIND.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The properties of stellar populations in the centers of nearby lenticular galaxies are investigated by means of 2D spectroscopy. All the galaxies are divided into 4 groups depending on the environment type; every subsample contains more than 10 galaxies. Clear distinctions between the mean stellar ages and abundance ratios are found both for the nuclei and for the bulges of the S0s in the different environments.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present our project on galaxy evolution in the environment of distant rich clusters aiming at disentangling the importance of specific interaction and galaxy transformation processes from the hierarchical evolution of field galaxies. Spatially resolved MOS spectra were gained with VLT/FORS to analyze the internal kinematics of disk galaxies. First results are shown for the clusters MS 1008.1–1224 ($z=0.30$), Cl 0303+1706 ($z=0.42$), and Cl 0413–6559 ($z=0.51$). Out of 35 late-type cluster members, 13 galaxies exhibit a rotation curve of the universal form rising in the inner region and passing over into a flat part. The other members have peculiar kinematics. The 13 cluster galaxies for which a maximum rotation velocity could be derived are distributed in the Tully-Fisher diagram very similarly to field galaxies from the FORS Deep Field with corresponding redshifts. The same is true for seven non-cluster galaxies observed in the cluster fields. The TF-cluster spirals do not show any significant luminosity evolution as might be expected from certain phenomena specific to clusters. Contrary to that, the disturbed kinematics of the non–TF cluster spirals indicate ongoing or recent interaction processes.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Here we present a self-consistent stationary solution for spherically symmetric winds driven by massive star clusters under the impact of radiative cooling. We demonstrate that cooling may modify drastically the distribution of temperature and the observational appearance of star cluster winds if the rate of injected energy approaches a critical value, and that the stationary wind solution does not exist if the energy deposition rate exceeds this limit.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We describe an ongoing programme using the FORS1 spectropolarimeter on the ESO-VLT to search for magnetic fields in Herbig Ae/Be stars. Our aim is to identify the pre-Main Sequence progenitors of magnetic Ap stars, and to trace the evolution of their magnetic fields at the earliest possible stages.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html