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  • 1
    Electronic Resource
    Electronic Resource
    The supernova remnant G78.2+2.1: New optical and X-ray observations (2000)
    Springer
    Astronomy letters 26 (2000), S. 77-87 
    Details
    ISSN: 1562-6873
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract New optical and X-ray observations of the supernova remnant (SNR) G78.2+2.1 are presented. CCD Hα observations with a Fabry-Perot interferometer attached to the 125-cm reflector at the Crimean Station of the Sternberg Astronomical Institute are used to obtain the radial-velocity field toward the SNR and in its vicinity. The brightness distribution and X-ray spectrum of the SNR are obtained from archival ROSAT and ASCA X-ray data. The X-ray image of G78.2+2.1 exhibits a shell structure (ΔR/R≃0.3) and is generally similar to its radio image; a comparison with the radio map at ν=1.4 GHz constructed from archival VLA data reveals the coincidence of features on scales of several arcminutes at the eastern boundary of G78.2+2.1. Weak X-ray emission (an outer shell or a halo of size ≃2°) has been identified for the first time far outside G78.2+2.1. The X-ray emission from G78.2+2.1 is shown to characterize a young adiabatic SNR [M X-ray ≃ 100 M ⊙, V s≃103km s−1, t≃(5–6)×103 years], which probably expands inside the cavity swept up by the progenitor's stellar wind. Searches for the corresponding radio structure are required to elucidate the nature of the outer X-ray shell or halo.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1134/1.20371
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  • 2
    Electronic Resource
    Electronic Resource
    A giant bipolar shell around the WO star in the galaxy IC 1613: Structure and kinematics (2000)
    Springer
    Astronomy letters 26 (2000), S. 153-161 
    Details
    ISSN: 1562-6873
    Keywords: interstellar medium ; stellar wind ; WR stars
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Observations of the nebula associated with the WO star in the galaxy IC 1613 are presented. The observations were carried out with a scanning Fabry-Perot interferometer in Hα using the 6-m Special Astrophysical Observatory telescope; narrow-band Hα and [O III]images were obtained with the 4-m KPNO telescope (USA). The monochromatic Hα image clearly reveals a giant bipolar shell structure outside the bright nebula S3. The sizes of the southeastern and northwestern shells are 112×77 and (186–192)×(214–224) pc, respectively. We have studied the object’s kinematics for the first time and found evidence for expansion of both shells. The expansion velocities of the southeastern and northwestern shells exceed 50 and 70 km s−1, respectively. We revealed a filamentary structure of the shells and several compact features in the S3 core. A scenario is proposed for the formation of the giant bipolar structure by the stellar wind from the central WO star located at the boundary of a “supercavity” in the galaxy’s H I distribution.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1134/1.20378
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  • 3
    Electronic Resource
    Electronic Resource
    Nebular complex in the region of Cas OB2 association; ring nebula Sh157 (1986)
    Springer
    Astrophysics and space science 121 (1986), S. 357-385 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract This paper presents the results of monochromatic [Oiii], [Nii], and [Sii] observations of ring nebula Sh157 around the star (WR + B0III) HD 219460 belonging to the Ba 3 cluster. A stratification of radiation typical for photoionization excitation has been revealed. The observations suggest that the Sh157 ring structure may arise as a result of the HD 219460 stellar wind blowing the surroundingHii region, and the bubble age is found to bet≃(2–5)×105 yr. Three outer envelopes have been distinguished: a weaker extended emission shell apparently blown out by the wind from B-stars of the Ba 3 cluster, and two dust shells which are likely to be associated with NGC 7510 and Cas OB2. The paper is also concerned with the discussion of young star aggregates Ba 3, NGC 7510, Cas OB1, OB2, OB4, OB5, OB7, and Cep OBI and the associatedHii regions, shells and supershells of gas and dust, molecular clouds, and supernova remnants which may be probable members of a single giant stellar complex where the star formation process is in progress.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00653708
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  • 4
    Electronic Resource
    Electronic Resource
    Ring nebulae associated with of stars: Statistics, classification, origin (1982)
    Springer
    Astrophysics and space science 87 (1982), S. 313-331 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The ring nebulae associated with galactic Of stars is considered on the grounds of the list of Of nebulae proposed by lozinskaya and Lomovsky (1982). Taking into account the selection effects, about 80% of Of stars are shown to be associated withHii regions and about 30–50% of these regions have shell structures. Four types of nebulae associated with Of stars are resolved: amorphousHii regions, ring-likeHii regions, wind-blown bubbles, and stellar ejectas. These types appear to be identical to the morphology of nebulae around WR stars proposed by Chu (1981). Observational data are presented and the nature of a number of Of ring nebulae of different types is discussed.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00648927
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  • 5
    Electronic Resource
    Electronic Resource
    Barrel-like supernova remnants (1990)
    Springer
    Astrophysics and space science 166 (1990), S. 277-287 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The origin of cylindrically-symmetric supernova remnants is discussed. The results of numerical simulations of two most distinguished barrel-like remnants SNR 1006 and G296.5+10.0 are presented.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF01094899
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  • 6
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    A family of cometary globules at the periphery of Cyg OB1: the star HBHA 3703-01 and the reflection nebula GM 2-39 (2013)
    Oxford University Press
    Details
    Publication Date: 2013-06-09
    Description: The interstellar medium in the region of a family of cometary globules including the reflection nebula GM 2–39 has been analysed based on our observations with a slit spectrograph, the results of our previous observations with a Fabry–Perot interferometer in the Hα line and Spitzer archival data (Hora et al.), together with CO microwave data (Leung & Thaddeus). The structure of the infrared emission of the globules, the velocity field of ionized gas in the Hα line and molecular gas in the CO line have been considered. We have detected a CO cavern around the eastern globules and faint high-velocity Hα features of the surrounding gas. The most probable sources of ionizing radiation and wind from stars of the Cyg OB1 association responsible for globule formation are proposed. Based on our multicolour photometry, it has been found that the brightest compact source in the southern ‘head’ of the cometary globule – the star HBHA 3703–01 (IRAS 20153+3850) – is a B(5–6)V star with E ( B  – V ) = 1.18 mag. A strong and broad Hα emission line was revealed in its spectrum. The spectral energy distribution of HBHA 3703–01 in the 0.44–24 μm range has been modelled. It is shown that the star has a hot dust envelope with T dust  = 1400 K and V  = 1.1. Additionally, the star HBHA 3703–01 illuminates the encompassing diffuse nebula GM 2–39 with a diameter of about 30 arcsec. With regard to all obtained observational data for HBHA 3703–01, this object may be classified as a Herbig Ae/Be star.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 7
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    Star-forming regions at the periphery of the supershell surrounding the Cyg OB1 association - I. The star cluster vdB 130 and its ambient gas and dust medium (2015)
    Oxford University Press
    Details
    Publication Date: 2015-10-15
    Description: Stellar population and the interstellar gas–dust medium in the vicinity of the open star cluster vdB 130 are analysed using optical observations taken with the 6 m telescope of the Special Astrophysical Observatory of Russian Academy of Sciences and the 125 cm telescope of the Sternberg Astronomical Institute, Lomonosov Moscow State University along with the data of Spitzer and Herschel . Based on proper motions and BV and JHK s Two Micron All Sky Survey photometric data, we select additional 36 stars as probable cluster members. Some stars in vdB 130 are classified as B stars. Our estimates of minimum colour excess, apparent distance modulus and the distance are consistent with young age (from 5 to 10 Myr) of the cluster vdB 130. We suppose the large deviations from the conventional extinction law in the cluster direction, with R V  ~ 4–5. The cluster vdB 130 appears to be physically related to the supershell around Cyg OB1, a cometary CO cloud, ionized gas and regions of infrared emission. There are a few regions of bright mid-infrared emission in the vicinity of vdB 130. The largest of them is also visible on Hα and [S ii ] emission maps. We suggest that the infrared blobs that coincide in projection with the head of the molecular cloud are H ii regions, excited by the cluster B stars. Some signatures of a shock front are identified between these IR-bright regions.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 8
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    Optical and infrared emission of H II complexes as a clue to the PAH life cycle (2014)
    Oxford University Press
    Details
    Publication Date: 2014-08-22
    Description: We present an analysis of optical spectroscopy and infrared aperture photometry of more than 100 H ii complexes in nine galaxies. Spectra obtained with the 6-m telescope of Special Astrophysical Observatory of the Russian Academy of Sciences are used along with archival data from Spitzer and several ground-based telescopes to infer a strength of polycyclic aromatic hydrocarbon (PAH) emission, age, properties of the UV radiation field, and metallicity of studied H ii complexes. Physical properties (age, radiation field parameters, metallicity) are related to the F 8 / F 24 ratio used as a proxy for the PAH abundance in order to reveal factors that may influence the PAH evolution in H ii complexes. The well-known correlation between the F 8 / F 24 ratio and metallicity is confirmed in the studied complexes. The infrared flux ratio also correlates with the [O iii ]5007/Hβ ratio which is often considered as an indicator of the radiation field hardness, but this correlation seems to be a mere reflection of a correlation between [O iii ]5007/Hβ and metallicity. In separate metallicity bins, the F 8 / F 24 ratio is found to correlate with an age of an H ii complex, which is estimated from the equivalent width of Hβ line. The correlation is positive for low-metallicity complexes and negative for high-metallicity complexes. Analysing various mechanisms of PAH formation and destruction in the context of found correlations, we suggest that PAH abundance is likely altered by the UV radiation within H ii complexes, but this is not necessarily due to their destruction. If PAHs can also form in H ii complexes due to some processes like aromatization, photodestruction, shattering and sputtering of very small grains, the net F 8 / F 24 ratio is determined by a balance between all these processes that can be different at different metallicities.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 9
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    The supergiant shell with triggered star formation in the dwarf irregular galaxy IC 2574: neutral and ionized gas kinematics (2014)
    Oxford University Press
    Details
    Publication Date: 2014-08-18
    Description: We analyse the ionized gas kinematics in the star formation regions of the supergiant shell (SGS) of the IC 2574 galaxy using observations made with the Fabry–Perot interferometer at the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences; the data of the H i Nearby Galaxy Survey (THINGS) are used to analyse the neutral gas kinematics in the area. We perform the ‘derotation’ of the Hα and H i data cubes and show its efficiency in the kinematics analysis. We confirm the SGS expansion velocity of 25 km s –1 obtained previously and conclude that the SGS is located at the far side of the galactic disc plane. We determine the expansion velocities, kinematic ages and the required mechanical energy input rates for four star formation complexes in the walls of the SGS; for those remaining, we give the limiting values of the above parameters. A comparison with the age and energy input of the stellar population of the complexes shows that sufficient energy is fed to all H ii regions except one. We discuss in detail the possible nature of this region and that of another region, which was believed to be a supernova remnant, according to radio observations. We have measured the expansion velocity of the latter and we can confirm its identification as an old supernova remnant. Our observations have allowed us to identify a faint diffuse Hα emission inside the SGS, which was not been previously observed.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 10
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    Complexes of triggered star formation in supergiant shell of Holmberg II (2016)
    Oxford University Press
    Details
    Publication Date: 2016-10-30
    Description: We report a detailed analysis of all regions of current star formation in the walls of the supergiant H i  shell (SGS) in the galaxy Holmberg II based on observations with a scanning Fabry–Perot interferometer at the Russian 6-m telescope. We compare the structure and kinematics of ionized gas with that of atomic hydrogen and with the stellar population of the SGS. Our deep Hα images and archival images taken by the Hubble Space Telescope demonstrate that current star formation episodes are larger and more complicated than previously thought: they represent unified star-forming complexes with sizes of several hundred pc rather than ‘chains’ of separate bright nebulae in the walls of the SGS. The fact that we are dealing with unified complexes is evidenced by identified faint shell-like structures of ionized and neutral gas which connect several distinct bright H ii  regions. Formation of such complexes is due to the feedback of stars with very inhomogeneous ambient gas in the walls of the SGS. The arguments supporting an idea about the triggering of star formation in SGS by the H i  supershells collision are presented. We also found a faint ionized supershell inside the H i  SGS expanding with a velocity of no greater than 10–15 km s –1 . Five OB stars located inside the inner supershell are sufficient to account for its radiation, although a possibility of leakage of ionizing photons from bright H ii  regions is not ruled out as well.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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