Search Results - (Author, Cooperation:J. N. Heasley)
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1S. Gezari ; R. Chornock ; A. Rest ; M. E. Huber ; K. Forster ; E. Berger ; P. J. Challis ; J. D. Neill ; D. C. Martin ; T. Heckman ; A. Lawrence ; C. Norman ; G. Narayan ; R. J. Foley ; G. H. Marion ; D. Scolnic ; L. Chomiuk ; A. Soderberg ; K. Smith ; R. P. Kirshner ; A. G. Riess ; S. J. Smartt ; C. W. Stubbs ; J. L. Tonry ; W. M. Wood-Vasey ; W. S. Burgett ; K. C. Chambers ; T. Grav ; J. N. Heasley ; N. Kaiser ; R. P. Kudritzki ; E. A. Magnier ; J. S. Morgan ; P. A. Price
Nature Publishing Group (NPG)
Published 2012Staff ViewPublication Date: 2012-05-12Publisher: Nature Publishing Group (NPG)Print ISSN: 0028-0836Electronic ISSN: 1476-4687Topics: BiologyChemistry and PharmacologyMedicineNatural Sciences in GeneralPhysicsPublished by: -
2Staff View
ISSN: 1572-946XSource: Springer Online Journal Archives 1860-2000Topics: PhysicsNotes: Abstract Color-magnitude diagrams are presented for the open cluster NGC 2158 and globular clusters Pal4 and NGC 1904.Type of Medium: Electronic ResourceURL: -
3Staff View
ISSN: 1573-093XSource: Springer Online Journal Archives 1860-2000Topics: PhysicsNotes: Abstract Observations of the Ca ii H, K, and infrared triplet lines are compared with theoretical predictions from the slab models of Heasley and Milkey (1976). While the theoretical models describe the hydrogen and helium emission spectra of quiescent prominences satisfactorily the predicted Ca ii lines are systematically too bright. The most likely reason for the discrepancy is the inapplicability of the symmetric slab prominence model for lines which become even moderately optically thick in prominences.Type of Medium: Electronic ResourceURL: -
4Staff View
ISSN: 1573-093XSource: Springer Online Journal Archives 1860-2000Topics: PhysicsNotes: Abstract The application of Unno's (1956) solution of the transfer equation for polarized radiation to the determination of thevector magnetic field is investigated. An analysis procedure utilizing non-linear least squares techniques is developed that allows one to automate the reduction of measured spectral profiles of the Stokes parameters to determine the field angles, strength as well as other parameters. The method is applied to synthetic spectra generated using a model solar atmosphere and yields results of remarkably high accuracy. The influence of additional factors upon determination of the vector field are also considered. These factors include effects of asymmetric profiles, magneto-optical effects, magnetic field gradients, unresolved field elements, scattered light, and instrumental noise.Type of Medium: Electronic ResourceURL: -
5Staff View
ISSN: 1573-093XSource: Springer Online Journal Archives 1860-2000Topics: PhysicsNotes: Abstract We present theoretical Ca ii K-line profiles and filtergram contrasts for several recent models of solar faculae. The line profiles vary greatly between models and between complete and partial frequency redistribution non-LTE calculations for any given model. The filtergram contrasts are relatively insensitive to the line formation theory which greatly simplifies the calculation for comparison with observations. All of the models considered exhibit K-line contrasts smaller than the mean value observed by Mehltretter.Type of Medium: Electronic ResourceURL: -
6Staff View
ISSN: 1476-4687Source: Nature Archives 1869 - 2009Topics: BiologyChemistry and PharmacologyMedicineNatural Sciences in GeneralPhysicsNotes: [Auszug] Previous imaging of PG1115 + 08 has been either by direct photography or speckle interferometry2'6; in all cases components B and C have been unresolved. Component A is resolved into two subcomponents (termed At and A2, north and south, respectively) separated by 0.5 arc s at a position angle of ...Type of Medium: Electronic ResourceURL: -
7Staff View
ISSN: 1573-093XSource: Springer Online Journal Archives 1860-2000Topics: PhysicsNotes: Abstract A theoretical study of the influence of propagating acoustic pulses in the solar chromosphere upon the line profiles of the Ca ii resonance and infrared triplet lines has been made. The major objective has been to explain the observed asymmetries seen in the cores of the H and K lines and to predict the temporal behavior of the infrared lines caused by passing acoustic or shock pulses. The velocities in the pulses, calculated from weak shock theory, have been included consistently in the non-LTE calculations. The results of the calculations show that these lines are very sensitive to perturbations in the background atmosphere caused by the pulses. Only minor changes in the line shapes result from including the velocities consistently in the line source function calculations. The qualitative changes in the line profiles vary markedly with the strength of the shock pulses. The observed differences in the K line profiles seen on the quiet Sun can be explained in terms of a spectrum of pulses with different wave-lengths and initial amplitudes in the photosphere.Type of Medium: Electronic ResourceURL: