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We present results of a survey of 14 star-forming regions from the Perseus spiral armin CS (2–1) and 13CO (1–0) lines with the Onsala Space Observatory 20 m telescope. Maps of 10 sources in both lines are obtained. For the remaining sources a map in just one line or a single-point spectrum is obtained. On the basis of newly obtained and published observational data we consider the relation between velocities of the “quasi-thermal” CS (2–1) line and 6.7 GHz methanol maser line in 24 high-mass star-forming regions in the Perseus arm. We show that, surprisingly, velocity ranges of 6.7 GHz methanol maser emission are predominantly red-shifted with respect to corresponding CS (2–1) line velocity ranges in the Perseus arm. We suggest that the predominance of the “red-shifted masers” in the Perseus arm could be related to the alignment of gas flows caused by the large-scalemotions in the Galaxy. Large-scale galactic shock related to the spiral structure is supposed to affect the local kinematics of the star-forming regions. Part of the Perseus arm, between galactic longitudes from 85° to 124° , does not contain blue-shifted masers at all. Radial velocities of the sources are the greatest in this particular part of the arm, so the velocity difference is clearly pronounced. 13CO (1–0) and CS (2–1) velocity maps of G183.35-0.58 show gas velocity difference between the center and the periphery of the molecular clump up to 1.2 km s?1. Similar situation is likely to occur in G85.40-0.00. This can correspond to the case when the large-scale shock wave entrains the outer parts of a molecular clump in motion while the dense central clump is less affected by the shock. 相似文献
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Multiple-method estimation of recharge rates at diverse locations in the North Carolina Coastal Plain, USA 总被引：1，自引：0，他引：1
Recharge rates determined at diverse study sites in a shallow, unconfined aquifer differed from one another depending on the
analytical method used and on each method’s applicability and limitations. Total recharge was quantified with saturated-zone
methods using water-table fluctuations at seven sites in North Carolina, USA and using groundwater-age dating at three of
the seven sites; at two of the sites, potential recharge was quantified with an unsaturated-zone method using Darcy’s law;
and at five of the sites, net recharge was quantified with a stream hydrograph-separation method using streamflow-recession
curves. Historical mean net recharge was 25 to 69% of the historical total recharge rates. The large disparity is attributed
to groundwater losses between recharge and discharge areas, primarily by evapotranspiration and seepage to underlying aquifers.
The spatial distribution of historical mean annual total recharge did not vary between landscape units, as suggested in a
previous study. Similarly, total recharge did not correlate significantly with mean annual rainfall, mean annual water table
depth, or the surficial soil properties of percent clay and bulk density. Total recharge did correlate significantly with
the surficial soil properties of percent sand and percent silt.
Résumé Les taux de recharge déterminés sur divers sites d’études dans un aquifère phréatique libre, varient les uns par rapport aux autres selon la méthode analytique utilisée et les limites et l’applicabilité de chaque méthode. La recharge totale a été quantifiée avec des méthodes en zone saturée utilisant les fluctuations des nappes sur sept sites de la Caroline du Nord, USA, et en utilisant les datations des eaux souterraines sur trois des sept sites ; sur deux des sites, la recharge potentielle a été quantifiée avec une méthode en zone non-saturée utilisant la loi de Darcy, et sur deux sites, la recharge nette a été quantifiée suivant une méthode de séparation des hydrographes de cours d’eau utilisant les courbes de récession du débit. La moyenne historique de la recharge nette est comprise entre 25 et 69% des taux historiques de recharge totale. L’importante disparité est attribuée aux pertes en eaux souterraines entre les zones de recharge et les zones d’exutoire, d’abord par évapotranspiration et ensuite par infiltration vers les aquifères sous-jacents. La distribution spatiale de la recharge historique moyenne annuelle et totale ne varie pas selon les unités paysagères, comme cela était suggéré dans une étude antérieure. De même, la recharge totale n’est pas corrélée significativement avec la moyenne annuelle des précipitations, la moyenne annuelle de la profondeur de la nappe, ou les propriétés de surface des sols que sont le pourcentage d’argile ou la densité apparente. La recharge totale est corrélée significativement avec les propriétés de surface du sol et les teneurs en sable et en silt.
Resumen Las tasas de recarga determinadas en diversos sitios de estudio en un acuífero somero no confinado difieren entre sí dependiendo del método analítico usado y de las limitaciones y aplicabilidad de cada método. Se cuantificó la recarga total con métodos de zona saturada usando fluctuaciones del nivel freático en siete sitios en Carolina del Norte, Estados Unidos, y usando datación de edades de agua subterránea en tres de los siete sitios; en dos de los sitios se cuantificó la recarga potencial con un método de zona no saturada usando la Ley de Darcy y en cinco de los sitios se cuantificó la recarga neta con el método de separación hidrográfica usando curvas de recesión de flujo en arroyos. La recarga neta media histórica varió entre 25 y 69% de las tasas de recarga total histórica. La diferencia tan grande se atribuye a pérdidas de agua subterránea entre áreas de descarga y recarga, principalmente por evapotranspiración y escurrimiento hacia acuíferos subyacentes. La distribución espacial de la recarga total anual media histórica no varió entre las unidades de paisaje, como ya se había sugerido en un estudio previo. De modo similar, la recarga total no guarda correlación significativa con la lluvia media anual, la profundidad media anual del nivel freático, o las propiedades superficiales del suelo, particularmente porcentaje de arcilla y densidad volumétrica. La recarga total si tuvo una correlación significativa con las propiedades superficiales del suelo tal como porcentaje de arena y porcentaje de limo.相似文献
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M. S. Kirsanova A. M. Sobolev M. Thomasson D. S. Wiebe L. E. B. Johansson A. F. Seleznev 《Monthly notices of the Royal Astronomical Society》2008,388(2):729-736
We present a picture of star formation around the H ii region Sh2-235 (S235) based upon data on the spatial distribution of young stellar clusters and the distribution and kinematics of molecular gas around S235. We observed 13 CO (1–0) and CS (2–1) emission toward S235 with the Onsala Space Observatory 20-m telescope and analysed the star density distribution with archival data from the Two Micron All-Sky Survey (2MASS). Dense molecular gas forms a shell-like structure at the southeastern part of S235. The young clusters found with 2MASS data are embedded in this shell. The positional relationship of the clusters, the molecular shell and the H ii region indicates that expansion of S235 is responsible for the formation of the clusters. The gas distribution in the S235 molecular complex is clumpy, which hampers interpretation exclusively on the basis of the morphology of the star-forming region. We use data on kinematics of molecular gas to support the hypothesis of induced star formation, and distinguish three basic types of molecular gas components. The first type is primordial undisturbed gas of the giant molecular cloud, the second type is gas entrained in motion by expansion of the H ii region (this is where the embedded clusters were formed) and the third type is a fast-moving gas, which might have been accelerated by winds from the newly formed clusters. The clumpy distribution of molecular gas and its kinematics around the H ii region implies that the picture of triggered star formation around S235 can be a mixture of at least two possibilities: the 'collect-and-collapse' scenario and the compression of pre-existing dense clumps by the shock wave. 相似文献
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Trofimova E. A. Zinchenko I. I. Zemlyanukha P. M. Thomasson M. 《Astronomy Reports》2020,64(3):244-258
Astronomy Reports - A survey of massive star forming regions in the lines of the lowest transitions of deuterated molecules DCN, DNC, DCO+, N2D+ in the 4 mm wavelength range was performed using the... 相似文献
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A. R. Breen S. J. Tappin C. A. Jordan P. Thomasson P. J. Moran R. A. Fallows A. Canals P. J. S. Williams 《Annales Geophysicae》2000,18(9):995-1002
Simultaneous observations of the slow solar wind off the southeast limb of the Sun were made in May 1999 using optical measurements from the C2 and C3 LASCO coronagraphs on board the SOHO spacecraft and radio-scattering measurements from the MERLIN and EISCAT facilities. The observations show the slow solar wind accelerating outwards from 4.5 solar radii (R), reaching a final velocity of 200–300 km s-1 by 25–30 R. The acceleration profile indicated by these results is more gentle than the average profile seen in earlier LASCO observations of larger scale features, but is within the variation seen in these studies. 相似文献
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Gene G. Byrd M. Thomasson K. J. Donner B. Sundelius T. Y. Huang M. J. Valtonen 《Celestial Mechanics and Dynamical Astronomy》1988,45(1-3):31-36
We study, theoretically and with N-body simulations, the formation of spiral patterns in retrograde galaxy encounters. A one-armed leading spiral dominates in a disk if the tidal perturbation from the companion is large and the disk is surrounded by a massive halo. Otherwise, a trailing pattern forms. The leading arm is made up of particles in slightly elongated orbits whose turning points outline the arm. The arm rotates opposite to the disk rotation. We have found one spiral galaxy, NGC4622, with a leading arm near its nucleus. From the literature, we find that very few spirals, if any, in a sample of strongly perturbed galaxies have leading arms. A possible reason for this is that few spiral galaxies have a halo with larger mass than the disk within the visible disk. 相似文献