The first galaxies: signatures of the initial starburst     

Jarrett L. Johnson †  Thomas H. Greif ‡  Volker Bromm  Ralf S. Klessen  Joseph Ippolito 《Monthly notices of the Royal Astronomical Society》2009,399(1):37-47

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Multiple clump structures within photoionized regions     

A. C. Raga  W. Henney  J. Vasconcelos  A. Cerqueira  A. Esquivel  A. Rodríguez-González 《Monthly notices of the Royal Astronomical Society》2009,392(3):964-968

We present 3D simulations of a system of four neutral clumps embedded in a photoionized region. In this system, we have three small clumps which partially shield a single, larger clump from the stellar ionizing photons. This flow evolves to form a neutral structure with a main body and three neutral 'columns' pointing towards the central star. Qualitatively, similar structures are seen in the 'Finger' of the Carina Nebula.  相似文献   

SOAR–OSIRIS observations of the Sh 2-307 H ii region: triggered star formation beyond the Solar Circle     

A. Roman-Lopes 《Monthly notices of the Royal Astronomical Society》2009,398(3):1368-1382

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Predictions of the extent of self-enrichment in oxygen of giant metal-poor H ii regions     

Aida Wofford 《Monthly notices of the Royal Astronomical Society》2009,395(2):1043-1054

In general, H  ii regions do not show clear signs of self-enrichment in products from massive stars  ( M ≥ 8 M_⊙)  . In order to explore why I modelled the contamination with Wolf–Rayet star ejecta of metal-poor  ( Z = 0.001)  H  ii regions, ionized either by a  10⁶ M_⊙  cluster of coeval stars (cluster 1) or by a cluster resulting from continuous star formation at a rate of  1 M_⊙ yr⁻¹  (cluster 2). The clusters have   Z = 0.001  and a Salpeter initial mass function from 0.1 to  120 M_⊙  . Independent one-dimensional constant density simulations of the emission-line spectra of unenriched H  ii regions were computed at the discrete ages 1, 2, 3, 4 and 5 Myr, with the photoionization code cloudy , using as input, radiative and mechanical stellar feedbacks predicted by the evolutionary synthesis code starburst99 . Each H  ii region was placed at the outer radius of the adiabatically expanding superbubble of Mac Low & McCray. For models with thermal and ionization balance time-scales of less than 1 Myr, and with oxygen emission-line ratios in agreement with observations, the volume of the superbubble and the H  ii region was uniformly and instantaneously polluted with stellar ejecta predicted by starburst99 . I obtained a maximum oxygen abundance enhancement of 0.025 dex, with cluster 1, at 4 Myr. It would be unobservable.  相似文献   

Triggered star formation and evolution of T-Tauri stars in and around bright-rimmed clouds     

Neelam Chauhan  A. K. Pandey  K. Ogura  D. K. Ojha  B. C. Bhatt  S. K. Ghosh  P. S. Rawat 《Monthly notices of the Royal Astronomical Society》2009,396(2):964-983

The aim of this paper is to quantitatively testify the ' small-scale sequential star formation ' hypothesis in and around bright-rimmed clouds (BRCs). As a continuation of the recent attempt by Ogura et al., we have carried out   BVI_c   photometry of four more BRC aggregates along with deeper re-observations of two previously observed BRCs. Again, quantitative age gradients are found in almost all the BRCs studied in the present work. Archival Spitzer /Infrared Array Camera data also support this result. The global distribution of near-infrared excess stars in each H  ii region studied here clearly shows evidence that a series of radiation-driven implosion processes proceeded in the past from near the central O star(s) towards the peripheries of the H  ii region. We found that in general weak-line T-Tauri stars (WTTSs) are somewhat older than classical T-Tauri stars (CTTSs). Also the fraction of CTTSs among the T-Tauri stars (TTSs) associated with the BRCs is found to decrease with age. These facts are in accordance with the recent conclusion by Bertout, Siess & Cabrit that CTTSs evolve into WTTSs. It seems that in general the equivalent width of Hα emission in TTSs associated with the BRCs decreases with age. The mass function (MF) of the aggregates associated with the BRCs of the morphological type 'A' seems to follow that found in young open clusters, whereas 'B/C'-type BRCs show significantly steeper MF.  相似文献   

Sh2-205 – II. Quiescent star-formation activity     

G. A. Romero †  C. E. Cappa ‡ 《Monthly notices of the Royal Astronomical Society》2009,395(4):2095-2102

We present a study of active star-forming regions in the environs of the H  ii region Sh2-205. The analysis is based on data obtained from point source catalogues and images extracted from the Two-Micron All-Sky Survey (2MASS), Midcourse Space Experiment ( MSX ) and IRAS surveys. Complementary data are taken from a CO survey. The identification of primary candidates for star-formation activity is made following colour criteria and a correlation with molecular gas emission.
A number of star-formation tracer candidates are projected on to two substructures of the H  ii region: SH 148.83–0.67 and SH 149.25–0.00. However, the lack of molecular gas related to these structures casts doubt on the nature of the sources. Additional infrared sources may be associated with the H  i shell centred at  ( l , b ) = (149°0', −1°30')  .
The most striking active area was found in connection with the H  ii region LBN 148.11–0.45, where star-formation candidates are projected on to molecular gas. The analytical model of the 'collect and collapse' process shows that star-formation activity could have been triggered by the expansion of this H  ii region.  相似文献   

Short-period variability in the Class II methanol maser source G12.89+0.49 (IRAS 18089−1732)     

S. Goedhart  M. C. Langa  M. J. Gaylard  D. J. van der Walt 《Monthly notices of the Royal Astronomical Society》2009,398(2):995-1010

Time series are presented for the Class II methanol maser source G12.89+0.49, which has been monitored for nine years at the Hartebeesthoek Radio Astronomy Observatory. The 12.2 and 6.7 GHz methanol masers were seen to exhibit rapid, correlated variations on time-scales of less than a month. Daily monitoring has revealed that the variations have a periodic component with a period of 29.5 d. The period seems to be stable over the 110 cycles spanned by the time series. There are variations from cycle to cycle, with the peak of the flare occurring anywhere within an 11 d window, but the minima occur at the same phase of the cycle. Time delays of up to 5.7 d are seen between spectral features at 6.7 GHz and a delay of 1.1 d is seen between the dominant 12.2 GHz spectral feature and its 6.7 GHz counterpart.  相似文献   

Hα measurements using DEFPOS/RTT150 Telescope： Instrumentation and observations     

Muhittin Sahan Ilhami Yegingil Nazim Aksaker 《中国天文和天体物理学报》2009,9(2)

To investigate the physical properties of HII regions and some PNe about 4' in size, a DEFPOS Fabry-Perot spectrometer has been redesigned and set up at the (Antalya/Bakirlitepe, Turkey), The spectrometer has a 4' circular field of view and a velocity resolution of 27.27 km s- 1 (a spectral resolving power of 11000) over a 200 km s-1 spectral window near Hα. This work presents the details of the newly redesigned inphysical results of our new Hα observations selected from the Reynolds et al. (2005) and Fich et al. (1990) papers. The DEFPOS system has been fully tested and the first observations of HII regions and PNe in the Galaxy are used to illustrate the power of the instrument. We feel that our first Fabry-Perot observations can provide a powerful tool for the study of objects with small angular size. In the future, we are planning to prepare a catalog including some physical properties such as radial velocity, line width, and intensity of some PNe and HII regions close to the 4' field of view.  相似文献   

Polar Vortex Response to Pacific Ocean Warming and Its Additive Nonlinearity with the Indian Ocean   总被引：1，自引：0，他引：1       下载免费PDF全文

LI Shuanglin 《大气和海洋科学快报》2010,3(6):303-307

A previous modeling study about Pacific Ocean warming derived polar vortex response signals, by subtracting those in the Indian Ocean warming experiments from those in the Indo-Pacific. This approach questions the resemblance of such an indirectly derived response to one directly forced by Pacific Ocean warming. This is relevant to the additive nonlinearity of atmospheric responses to separated Indian and Pacific Ocean forcing. In the present study, an additional set of ensemble experiments are performed by prescribing isolated SST forcing in the tropical Pacific Ocean to address this issue. The results suggest a qualitative resemblance between responses in the derived and additional experiments. Thus, previous findings about the impact of Indian and Pacific Ocean warming are robust. This study has important implications for future climate change projections, considering the non-unanimous warming rates in tropical oceans in the 21st century. Nevertheless, a comparison of present direct-forced experiments with previous indirect-forced experiments suggests a significant additive nonlinearity between the Indian and Pacific Ocean warmings. Further diagnosis suggests that the nonlinearity may originate from the thermodynamic processes over the tropics.  相似文献   

Tropical cyclones and polar lows: Velocity,size, and energy scales,and relation to the 26°C cyclone origin criteria     

G. S. GOLITSYN 《大气科学进展》2009,26(3):585-598

The goal of this paper is to quantitatively formulate some necessary conditions for the development of intense atmospheric vortices. Specifically, these criteria are discussed for tropical cyclones (TC) and polar lows (PL) by using bulk formulas for fluxes of momentum, sensible heating, and latent heating between the ocean and the atmosphere. The velocity scale is used in two forms: (1) as expressed through the buoyancy flux b and the Coriolis parameter l_c for rotating fluids convection, and (2) as expressed with the cube of velocity times the drag coefficient through the formula for total kinetic energy dissipation in the atmospheric boundary layer. In the quasistationary case the dissipation equals the generation of the energy. In both cases the velocity scale can be expressed through temperature and humidity differences between the ocean and the atmosphere in terms of the reduced gravity, and both forms produce quite comparable velocity scales. Using parameters b and l_c, we can form scales of the area and, by adding the mass of a unit air column, a scale of the total kinetic energy as well. These scales nicely explain the much smaller size of a PL, as compared to a TC, and the total kinetic energy of a TC is of the order 10¹⁸-10¹⁹ J. It will be shown that wind of 33 m s^-1 is produced when the total enthalpy fluxes between the ocean and the atmosphere are about 700 W m^-2 for a TC and 1700 W m^-2 for a PL, in association with the much larger role of the latent heat in the first case and the stricter geostrophic constraints and larger static stability in the second case. This replaces the mystical role of 26^oC as a criterion for TC origin. The buoyancy flux, a product of the reduced gravity and the wind speed, together with the atmospheric static stability, determines the rate of the penetrating convection. It is known from the observations that the formation time for a PL reaching an altitude of 5--6 km can be only a few hours, and a day, or even half a day, for a TC reaching 15--18 km. These two facts allow us to construct curves on the plane of T^s and ΔT=T_s-T_a to determine possibilities for forming an intense vortex. Here, T_a is the atmospheric temperature at the height z=10 m. A PL should have ΔT>20^oC in accordance with the observations and numerical simulations. The conditions for a TC are not so straightforward but our diagram shows that the temperature difference of a few degrees, or possibly even a fraction of a degree, might be sufficient for TC development for a range of static stabilities and development times.  相似文献