In this paper we present some preliminary results of a 3-mm (86 GHz) radio continuum survey of selected Seyfert galaxies made with the Berkley-Maryland Illinois Millimeter Array (BIMA) in D configuration. The images shown here have spatial resolutions of about two arcminutes after gaussian tapering. At this observing wavelength, we expect to have a negligible non-thermal emission as the spectra is certainly dominated by free-free radio emission. We have measured flux densities and 3 mm luminosities which agree with a thermal blackbody spectra expected from data obtained with the IRAS satellite at wavelengths shorter than 80 μm. Data is presented for NGC3982, NGC5597, NGC5253, NGC1667, and NGC2997 and the main astrophysical consequences of such studies are discussed in this poster. We also argue that radio continuum at millimeter wavelengths is a better observational tool to study the star-formation in active galaxies than conventional infrared photometry.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present the results of L-band spectroscopic observations of local bright ULIRGs, performed with ISAAC at VLT. The excellent sensitivity of the telescope and instrument provided spectra of unprecedented quality for this class of objects, which allowed a detailed study of the relative AGN/starburst contribution to the energy output, and of the composition of the circumnuclear absorber. A new mid-infrared diagnostic diagram is proposed, in which starbursts and AGNs are clearly separated.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

An analysis of the distribution of coronal brightness in the UV radiation according to SOHO/EIT in the wavelengths 171Å, 195Å and 304Å was carried out. A change of coronal brightness at the heights $1.02R-1.20R$ radius of the Sun was considered during 1996-2003. The distribution of brightness of the corona at the various heights depends on the phase of the solar cycle. Brightness of the corona at the heights more 1.05R in the wavelengths 171Å and 195Å has the greatest brightness during an epoch of the maximum activity. Brightness of the internal corona at the heights less $1.05R$ has the lowered brightness during this period. The maximum intensity of the corona 304Å was observed in the maximum activity at all heights. Comparison brightness of the corona with the number bright points in UV was carried out. For this purpose the bright points in the wavelength 304Å were allocated on the solar disk of the daily observations. The number of the bright points has the maximum on the phase of the minimum activity while the area of the bright regions has maximum in the maximum activity.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

HD 34282 has been found to pulsate during a systematic search for short-term photometric variability in Herbig Ae/Be stars with the goal of determining the position and size of the pre-Main Sequence instability strip. Simultaneous Strömgren photometry is used in the frequency analysis, yielding two frequencies with values of $\nu_1 = 79.5$ and $\nu_2 = 71.3$ cycle ${\rm d}^{-1}$. The main period, with a value of 18.12 min, represents the shortest period observed up to now for a $\delta$ Scuti-type pulsator. A preliminary seismic modelling, including instability predictions and rotation effects, has been attempted. Both, Main Sequence and pre-Main Sequence models predict modes in the range of 56 to 82 cycle ${\rm d}^{-1}$ (between 648 and 949 $\mu{\rm Hz}$), corresponding to oscillations of radial order n from 6 to 8. The mode identification is not discriminating due to the large error bars attached to the data, therefore, all possible non-radial and radial modes up to $\ell = 3$ are compatible with the observed oscillations.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

In this study we use preliminary atmospheric parameters for the A0 Ib supergiant $\eta$ Leo ($T_{\rm eff}, \log g$ and microturbulent velocity) to provide initial estimates of the elemental abundances from S II, Ti II, Cr II, Fe I and Fe II lines by using spectrograms with a two pixel resolution of 0.072 Å and signal-to-noise ratio $\ge$ 200 taken at the Dominion Astrophysical Observatory.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

An erupting prominence seen by SOHO/EIT was tracked into the field of view of the LASCO C2 and C3 coronagraphs where it developed into the core of a structured CME. The erupting prominence was deflected by an angle of $\sim 20^{\circ}$ towards the north pole whereas the consequent core of the CME and it's leading edge propagated in the outer corona at constant position angle. The prominence material underwent a constant acceleration phase until a height of $\sim$1.5 solar radii before it started to decelerate up to a distance of 5.0 solar radii. An inflow of plasma with a speed of about 70-80 km/s was discovered in the EIT observations at a height of 1.5-1.2 solar radii in the course of the prominence eruption, matching in time the prominence deceleration phase. The downflowing material followed a curved path, suggestive of the apex of a contracting magnetic loop sliding down along other field lines.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present theoretical Fe I-III emission-line strengths for physical conditions typical of Active Galactic Nuclei with Broad-Line Regions. We can satisfactorily reproduce the empirical UV Fe II-III emission-line template of Vestergaard & Wilkes (2001) for the prototypical narrow-line Seyfert 1 galaxy I Zw 1, although a number of detailed discrepancies remain.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The results of research of halfwidhts ($\Delta\lambda$) and intensities (W) of Fe X $\lambda 6374 \AA$ and Fe XIV $\lambda 5303\AA$ spectral lines using observations obtained with the Large coronagraph of the Sayan observatory in 1968-1983 show the inverse correlation between $\Delta\lambda$ and W always exists for Fe X $\lambda 6374 \AA$; it takes place at all latitudes at the same height as well as with height irrespectively of activity level. For Fe XIV $\lambda 5303 \AA$ this correlation varies from direct to inverse depending on activity level. It is shown that relation type between $\Delta\lambda$ and W for different spectral lines is determined by different coronal structurednesses in these lines.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Using Kurucz's ATLAS9 model atmospheres I performed LTE fine analyses of the supergiants 4 Lac and $\nu$ Cep. The spectra were obtained at 1.22-m telescope of the Dominion Astrophysical Observatory (DAO) by Saul J. Adelman. The atmospheric parameters were derived using the wings of ${\rm H}\beta$ and ${\rm H}\gamma$ profiles for each star, and from Fe I/II, Fe II/III, and Si II/III equilibria for 4 Lac, and from Fe I/II and Cr I/II equilibria for $\nu$ Cep. A microturbulence of $2.7\,{\rm km\,s}^{-1}$ for 4 Lac was found from Fe II lines while a mean value of $5.2\,{\rm km\,s}^{-1}$ for $\nu$ Cep from Cr II, Ti II and Fe II lines. The rotational and macroturbulent velocities are, respectively, $14\pm2{\rm km\,s}^{-1}$ and $15\pm 2\,{\rm km\,s}^{-1}$ for 4 Lac, and $26 \pm 2{\rm km\,s}^{-1}$ and $12 \pm 2{\rm km\,s}^{-1}$ for $\nu$ Cep. Their He, CNO and light element abundances are solar or overabundant while their iron peak and heavy element abundances are solar or underabundant. The derived results show that 4 Lac has nuclearly processed matter in its photosphere while $\nu$ Cep does not.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We have studied how the active nucleus of the Seyfert 2 galaxy NGC 1068 influences the chemistry of its 200 pc circumnuclear disk of molecular gas (CND). Results from new observations made with the IRAM 30m telescope have served for deriving abundances of molecular species such as SiO, CN, HCO+, HOC+, H13CO+ and HCO. These estimates are complemented with a re-evaluation of abundances of HCN, CS and CO, based on previously published observations. We report on the first detection of significant SiO emission in the CND of NGC 1068. We also report on the first extragalactic detection of the reactive ion HOC+. Our conclusions favour an overall scenario where the CND of NGC 1068 has become a giant X-ray Dominated Region (XDR).To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

A short compilation of results of spectral observations of nonthermal velocities $\xi$ in a wide range of temperatures in X-ray, EUV, UV and visual wave-lengths has been made. Relationship between the $\xi$ and electron temperature T for chromosphere, quiet and active corona, coronal holes (CHs) and flaring plasma is considered.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The progenitors of magnetic white dwarfs are believed to be magnetic Ap and Bp stars because the fields in these stars are structured and are present in the stellar core. As in Ap/Bp stars the magnetic fields in white dwarfs are, in most cases, dipolar or quadrupolar with various offsets. Although the present space density of Ap/Bp progenitors would be sufficient to account for the density of magnetic white dwarfs in young populations such as found in the Palomar-Green survey, we show that it would be insufficient to generate the density of known magnetic white dwarfs in the older solar neighborhood. Assuming magnetic flux conservation during the final stages of evolution, we find that Ap/Bp stars would evolve into white dwarfs with magnetic fields exceeding $10^7$ G, assuming a minimum polar field of 200 G in Ap/Bp stars, thereby leaving many magnetic white dwarfs with lower fields without likely progenitors.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We have analyzed the position angle (PA) differences between radio jets and dust distributions in the centers of Fanaroff & Riley Type 1 (FRI) radio galaxies. We model the observed PA differences to infer the three-dimensional relative orientation of jet and dust. Our main conclusion is that there is a dichotomy in dust-jet-galaxy orientation both in projection and in three-dimensional space. The orientation dichotomy can explain the contradictory results obtained in previous studies. We briefly mention scenarios that might explain the dichotomy.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

In this paper we present results of a detailed morphological and radio polarization study of the nearby radio galaxy 3C33.1 (4C72.01, 0106+729, z = 0.18) made with the Very Large Array at 18 and 21 cm. Recently, this galaxy has been re-classified within a sample of large core-dominated radio sources and it has an exceedingly high projected linear size of ∼450 kpc. The jet shows little Faraday rotation, with rotation measures |RM|<20 rad m−2, whereas the hotspots exhibit higher values. The low rotation measures indicate that this radio source has a visible jet, which can be a naked jet or stripped from a dense environment. A spectral ageing analysis, based on syncrotron power losses arguments of the integrated spectra, suggest that the radio structure is not younger than 20 Myrs. Further observational properties of this radio galaxy are also discussed.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We calculate the synthetic spectra of TT Hya, an Algol-type eclipsing binary system which contains an A-type primary surrounded by a disc, and an evolved secondary which fills its Roche lobe. A new code SHELLSPEC was developed to solve the simple radiative transfer along the line of sight propagating through the 3D moving medium in LTE. The synthetic spectra are then compared with the observed ones which enable us to derive independent constraints on the behavior of the state quantities, the velocity field and the geometry of the disc.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

There are dozen instruments successfully operating aboard the solar satellite CORONAS-F, which was launched in the summer of 2001. Among them are two (Polish-led) Bragg crystal spectrometers – RESIK and Diogeness – recording solar flare and active region spectra. A short description of the CORONAS-F satellite operation is presented together with that of the two Polish spectrometers, stressing their unique characteristics. The average spectra have been derived and shown here, covering the wavelength range between 3 Å and 7 Å. Future steps in the analysis of the large database collected are outlined.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Specific features of magnetic reconnection in solar flares are briefly reviewed and illustrated. In particular, the large-scale structure and dynamics of large flares are interpreted in terms of the rainbow reconnection model. The role of the betatron effect in collapsing magnetic traps is considered.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We pursue the dynamics of dusty gas clouds that are blown out of circumnuclear starburst regions, taking into consideration the growth of clouds by inelastic cloud-cloud collision and the resultant change of the optical depth. As a result, we find that the clouds originating in the circumnuclear starburst can contribute to the obscuration to produce type 2 Seyfert galaxies. Also, it is shown that, if the AGN luminosity overwhelms the starburst one, almost all clouds are ejected from the galaxy by the radiation pressure of the AGN, resulting in the formation of quasar-like objects.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We report irregular changes in the line profiles of Deneb, and suggest that they represent part of the mechanism causing the stellar wind.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We describe two flares of GOES class M5.7 and 1.5 which were observed simultaneously by RHESSI (Ramaty High Energy Solar Spectroscopic Imager) and NoRH (Nobeyama Radio Heliograph). Both flares exhibit slow motions suggestive of changing magnetic shear, loop expansion, or gradual reconnection. One flare is clearly a coronal hard X-ray and microwave flare.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html