اشترك بالحزمة الذهبية واحصل على وصول غير محدود شمرا أكاديميا
تسجيل مستخدم جديدThe hyperyoung HII region in G24.78+0.08 A1
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M.T. Beltran
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Context. G24.78+0.08 A1 is a 20 Msun star surrounded by a hypercompact (HC) HII region, driving a CO bipolar outflow, and located at the center of a massive rotating toroid undergoing infall towards the HC region. Recent water maser observations suggest that the HC region is expanding and accretion onto the star is halted. Aims. This study aims to confirm the expansion scenario proposed for the HC region on the basis of recent H2O maser observations. Methods. We carried out continuum VLA observations at 1.3cm and 7mm with the A array plus Pie Town configuration to map the HC region towards G24 A1. Results. The emission of the HC region has been resolved and shows a ring shape structure. The profiles of the emission obtained by taking slices at different angles passing through the barycenter of the HC region confirm the shell structure of the emission. The ratio between the inner and the outer radius of the shell, Ri/Ro, derived fitting the normalized brightness temperature profile passing through the peak of the 7mm emission, is 0.9, which indicates that the shell is thin. The deconvolved outer radius estimated from the fit is 590 AU. These results imply that the HC region in G24 A1 cannot be described in terms of a classical, homogeneous HII region but is instead an ionized shell. This gives support to the model of an expanding wind-driven, ionized shell suggested by the kinematics and distribution of the H2O masers associated with the HC region. According to this model, the HC region is expanding on very short times scales, 21-66 yr.
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The study of hyper-compact (HC) or ultra-compact (UC) HII regions is fundamental to understanding the process of massive (> 8 M_sun) star formation. We employed Atacama Large Millimeter/submillimeter Array (ALMA) 1.4 mm Cycle 6 observations to invest
igate at high angular resolution (~0.050, corresponding to 330 au) the HC HII region inside molecular core A1 of the high-mass star-forming cluster G24.78+0.08. We used the H30alpha emission and different molecular lines of CH3CN and 13CH3CN to study the kinematics of the ionized and molecular gas, respectively. At the center of the HC HII region, at radii <~500 au, we observe two mutually perpendicular velocity gradients, which are directed along the axes at PA = 39 deg and PA = 133 deg, respectively. The velocity gradient directed along the axis at PA = 39 deg has an amplitude of 22 km/s mpc^(-1), which is much larger than the others, 3 km/s mpc^(-1). We interpret these velocity gradients as rotation around, and expansion along, the axis at PA = 39 deg. We propose a scenario where the H30alpha line traces the ionized heart of a disk-jet system that drives the formation of the massive star (~20 M_sun) responsible for the HC HII region. Such a scenario is also supported by the position-velocity plots of the CH3CN and 13CH3CN lines along the axis at PA = 133 deg, which are consistent with Keplerian rotation around a 20 M_sun star. Toward the HC HII region in G24.78+0.08, the coexistence of mass infall (at radii of ~5000 au), an outer molecular disk (from <~4000 au to >~500 au), and an inner ionized disk (<~500 au) indicates that the massive ionizing star is still actively accreting from its parental molecular core. To our knowledge, this is the first example of a molecular disk around a high-mass forming star that, while becoming internally ionized after the onset of the HII region, continues to accrete mass onto the ionizing star.
Over a timescale of a few years, an observed change in the optically thick radio continuum flux can indicate whether an unresolved H II region around a newly formed massive star is changing in size. In this Letter we report on a study of archival VLA
observations of the hypercompact H II region G24.78+0.08 A1 that shows a decrease of ~ 45 % in the 6-cm flux over a five year period. Such a decrease indicates a contraction of ~ 25 % in the ionized radius and could be caused by an increase in the ionized gas density if the size of the H II region is determined by a balance between photoionization and recombination. This finding is not compatible with continuous expansion of the H II region after the end of accretion onto the ionizing star, but is consistent with the hypothesis of gravitational trapping and ionized accretion flows if the mass-accretion rate is not steady.
We present the results of high angular resolution millimeter observations of gas and dust toward G31.41+0.31 and G24.78+0.08, two high-mass star forming regions where four rotating massive toroids have been previously detected by Beltran et al. (2004
). The CH3CN (12-11) emission of the toroids in G31.41+0.31 and core A1 in G24.78+0.08 has been modeled assuming that it arises from a disk-like structure seen edge-on, with a radial velocity field. For G31.41+0.31 the model properly fits the data for a velocity v_rot~1.7 km/s at the outer radius R_out~13400 AU and an inner radius R_inn~1340 AU, while for core A1 in G24.78+0.08 the best fit is obtained for v_rot~2.0 km/s at R_out~7700 AU and R_inn~2300 AU. Unlike the rotating disks detected around less luminous stars, these toroids are not undergoing Keplerian rotation. From the modeling itself, however, it is not possible to distinguish between constant rotation or constant angular velocity, since both velocity fields suitably fit the data. The best fit models have been computed adopting a temperature gradient of the type T proportional R^{-3/4}, with a temperature at the outer radius T_out~100 K for both cores. The M_dyn needed for equilibrium derived from the models is much smaller than the mass of the cores, suggesting that such toroids are unstable and undergoing gravitational collapse. The collapse is also supported by the CH3^{13}CN or CH3CN line width measured in the cores, which increases toward the center of the toroids. The estimates of v_inf and dot M_acc are ~2 km/s and 3x10^{-2} M_sun/yr for G31.41+0.31, and ~1.2 km/s and ~9x10^{-3} M_sun/yr for G24.78+0.08 A1. Such large accretion rates could weaken the effect of stellar winds and radiation pressure and allow further accretion on the star.
Context. This study is part of a large project to study the physics of accretion and molecular outflows towards a selected sample of high-mass star-forming regions that show evidence of infall and rotation from previous studies. Aims. We wish to make
a thorough study at high-angular resolution of the structure and kinematics of the HMCs and corresponding molecular outflows in the high-mass star-forming region G24.78+0.08. Methods. We carried out SMA and IRAM PdBI observations at 1.3 and 1.4 mm, respectively, of dust and of typical high-density and molecular outflow tracers with resolutions of <1. Complementary IRAM 30-m 12CO and 13CO observations were carried out to recover the short spacing information of the molecular outflows. Results. The millimeter continuum emission towards cores G24 A1 and A2 has been resolved into 3 and 2 cores, respectively, and named A1, A1b, A1c, A2, and A2b. All these cores are aligned in a southeast-northwest direction coincident with that of the molecular outflows detected in the region, which suggests a preferential direction for star formation in this region. The masses of the cores range from 7 to 22 Msun, and the rotational temperatures from 128 to 180 K. The high-density tracers have revealed the existence of 2 velocity components towards A1, one of them peaks close to the position of the millimeter continuum peak and of the HC HII region, and is associated with the velocity gradient seen in CH3CN towards this core, while the other one peaks southwest of core A1 and is not associated with any millimeter continuum emission peak. The position-velocity plots along outflow A and the 13CO averaged blueshifted and redshifted emission indicate that this outflow is driven by core A2.
We present spectroscopic observations for six emission-line objects projected onto the Virgo cluster. These sources have been selected from narrow band (Halpha+[NII]) images showing faint detectable continuum emission and EW>100 Angstrom. Five of the
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