Save Astro World

This is a single-factor analysis of the variance of the average quasimonochromatic magnitudes of Fomalhaut, α PsA, in the
325-1080

The temperature distribution with depth in the atmosphere of the magnetic star HD21699 is modelled for each observed rotational
phase using Hδ line profiles obtained with a signal to noise ratio S/N = 1000. The observed temperature distributions were
averaged within and outside the region of the magnetic spots. It appears that these average temperatures are equal to within
the limits of error. This shows that the magnetic field does not affect the physical condition of the matter in the star and
does not disturb its thermodynamic state.

Content Type Journal ArticleCategory Brief CommunicationsPages 1-4DOI 10.1007/s10511-012-9217-xAuthors
Yu. V. Glagolevskij, Special Astrophysical Observatory, Caucasus Mountains, RussiaG. A. Chuntonov, Special Astrophysical Observatory, Caucasus Mountains, RussiaA. V. Shavrina, Main Astronomical Observatory, Kyiv, Ukraine

Journal AstrophysicsOnline ISSN 1573-8191Print ISSN 0571-7256

This is an examination of two groups of stars, one of which contains a trapezium-type system consisting of four stars, while
the second is made up of three stars, which are also part of a trapezium-type system. The two groups are located in the CMa
OB1 association and contain cometary nebulae. Data on ¹²CO(1-0) observations of the molecular cloud connected with the first group of stars are presented. The central portion of
the molecular cloud is moving toward us. This may be a consequence of the presence of a strong flow inside the cloud produced
by the star-formation region.

Content Type Journal ArticlePages 1-6DOI 10.1007/s10511-012-9215-zAuthors
A. L. Gyulbudaghian, V. A. Ambartsumyan Byurakan Astrophysical Observatory, Byurakan, Armenia

Journal AstrophysicsOnline ISSN 1573-8191Print ISSN 0571-7256

This is a study of the stability of strange dwarfs, superdense stars with a small self-confining core (M

_core
 < 0.02

The methods of panoramic (3D) spectroscopy are used by us in a detailed study of galaxies with ongoing star formation chosen
from among objects in seven selected fields of the Second Byurakan Survey (SBS). This article deals with the irregular galaxy
SBS 1202 + 583, which our classification scheme identifies as being in a continuous phase of star formation. Observations
were made with the panoramic spectrographs MPFS at the 6-m telescope of the Special Astrophysical Observatory (SAO) of the
Russian Academy of Sciences and VAGR at the 2.6-m telescope of the Byurakan Astrophysical Observatory (BAO) in Armenia. The
data are used to construct maps of the radiative fluxes in the continuum and various emission lines. Special attention is
devoted to analyzing the emission in the Hα hydrogen recombination line and in the forbidden low-ionization doublets of nitrogen [NII] λλ6548, 6583 and sulfur [SII] λλ6716, 6731, and the ratios of the intensities of the forbidden lines to Hα. The observable characteristics (size, Hα fluxes, etc.) of nine HII regions are studied. The estimated current rates of star formation in the individual HII regions
based on the Hα fluxes lie within the range of 0.3-1.2_⨀ M /year. The dependence of the ratio of the intensities of the emission in these above mentioned forbidden doublets on the
rate of star formation in the HII regions is found.

Content Type Journal ArticlePages 1-13DOI 10.1007/s10511-012-9209-xAuthors
S. A. Hakopian, V. A. Ambartsumyan Byurakan Astrophysical Observatory, Byurakan, ArmeniaS. K. Balayan, V. A. Ambartsumyan Byurakan Astrophysical Observatory, Byurakan, ArmeniaS. N. Dodonov, Special Astrophysical Observatory, Nizhnij Akhyz, RussiaA. V. Moiseev, Special Astrophysical Observatory, Nizhnij Akhyz, RussiaA. A. Smirnova, Special Astrophysical Observatory, Nizhnij Akhyz, Russia

Journal AstrophysicsOnline ISSN 1573-8191Print ISSN 0571-7256

The luminosity function (LF) of galaxies in different environments is studied. A method proposed by the author is used to
determine the LF of galaxies. It is found that the luminosity functions of galaxies of different morphological types in single
galaxies and small groups do not differ greatly. The luminosity functions of galactic clusters differ greatly from the analogous
functions for other systems. A relatively large number of faint galaxies is observed in clusters. Groups with low dispersions
in their radial velocities and with small average pairwise distances between the members contain relatively many faint galaxies
and relatively few bright galaxies compared to groups with large dispersions in their radial velocities and large average
pairwise distances between members. This applies to elliptical and lenticular galaxies, as well as to spiral and irregular
galaxies.

Content Type Journal ArticlePages 1-11DOI 10.1007/s10511-012-9212-2Authors
A. P. Mahtessian, V. A. Ambartsumyan Byurakan Astrophysical Laboratory, Byurakan, Armenia

Journal AstrophysicsOnline ISSN 1573-8191Print ISSN 0571-7256

43 stellar objects with Hα emission are discovered by slitless spectroscopy in a 14’ × 14′ area near the nebula GM 2-41 located
in the HII region DR 15 at the southern edge of the Cyg OB2 association. Emission is detected for the first time for 30 of
these objects. Based on VI and JHK photometric data, the overwhelming majority of these objects are classified as young stellar
objects in spectral classes F7-M3 with ages of ~1 Myr. The stars are distributed nonuniformly and form two groups which have
the same coordinates as the UCHII regions G0.79 + 0.3 and G79.2 + 0.4.

Content Type Journal ArticlePages 1-11DOI 10.1007/s10511-012-9214-0Authors
E. H. Nikoghosyan, V. A. Ambartsumyan Byurakan Astrophysical Observatory, Byurakan, ArmeniaT. Yu. Magakian, V. A. Ambartsumyan Byurakan Astrophysical Observatory, Byurakan, ArmeniaT. A. Movsessian, V. A. Ambartsumyan Byurakan Astrophysical Observatory, Byurakan, Armenia

Journal AstrophysicsOnline ISSN 1573-8191Print ISSN 0571-7256

A series of numerical experiments is carried out to simulate the dynamical evolution of groups of galaxies in different models
of gravitation. The simulation results are compared with observations of the Local Group and of the CenA/M83 and M81/M82 galactic
groups. It is found that the LCDM model and the MOND (Modified Newtonian Dynamics) model are in substantially better agreement
with the observations than the other two models examined here. The dispersion in the velocities relative to Hubble’s law in
these models is small, but the MOND model yields slightly elevated values. For initial conditions close to virial equilibrium,
the mean square deviations in the velocities of the galaxies are ~30

Using an apparent-magnitude limited Main galaxy sample of the Sloan Digital Sky Survey Data Release 7(SDSS DR7), we investigate
the correlation between morphologies and luminosity for the Main galaxy sample. Our Main galaxy sample is divided into two
classes: Main galaxies only with TARGET_GALAXY flag (bestPrimtarget = 64), and ones also with other flags. It is found that
for the second class Main galaxies, the early-type proportion monotonously increases with increasing luminosity nearly in
the whole luminosity region. But for the first class Main galaxies, the early-type proportion increases with increasing luminosity
only within a certain luminosity region (−22.2 < M

_r
 < −19.8). In the high luminosity region (M

_r
 < −22.2), the early-type proportion of the first class Main galaxies even decreases dramatically with increasing luminosity.
We also analyze the correlation between morphologies and luminosity of galaxies around the peak of the redshift distribution
( 0.07 ≤ z ≤ 0.08 ). In such a narrow redshift region, we still observe strong correlation between morphologies and luminosity,
which shows that this correlation is fundamental.

Content Type Journal ArticlePages 1-8DOI 10.1007/s10511-012-9213-1Authors
Xin-Fa Deng, School of Science, Nanchang University, Nanchang, ChinaXiao-Xia Qian, School of Science, Nanchang University, Nanchang, ChinaCheng-Hong Luo, School of Science, Nanchang University, Nanchang, ChinaPing Wu, School of Science, Nanchang University, Nanchang, China

Journal AstrophysicsOnline ISSN 1573-8191Print ISSN 0571-7256

The results of analysis of approximately 3