Zobrazeno 1 - 10
of 724
pro vyhledávání: '"Harrington, D. P."'
Autor:
Schad, T. A., Fehlmann, A., Dima, G. I., Kuhn, J. R., Scholl, I. F., Harrington, D., Rimmele, T., Tritschler, A., Paraschiv, A. R.
We report commissioning observations of the Si X 1430 nm solar coronal line observed coronagraphically with the Cryogenic Near-Infrared Spectropolarimeter (Cryo-NIRSP) at the National Science Foundation's Daniel K. Inouye Solar Telescope (DKIST). The
Externí odkaz:
http://arxiv.org/abs/2402.09632
Autor:
Harrington, D. M., Sueoka, S. R.
Modern observatories and instruments require optics fabricated at larger sizes with more stringent performance requirements. The Daniel K. Inouye Solar Telescope will be the world's largest solar telescope at 4.0 m aperture delivering a 300 Watt beam
Externí odkaz:
http://arxiv.org/abs/1811.10321
Autor:
Berdyugina, S. V., Harrington, D. M., Kuzmychov, O., Kuhn, J. R., Hallinan, G., Kowalski, A. F., Hawley, S. L.
We report the first direct detection of a strong, 5 kG magnetic field on the surface of an active brown dwarf. LSR J1835+3259 is an M8.5 dwarf exhibiting transient radio and optical emission bursts modulated by fast rotation. We have detected the sur
Externí odkaz:
http://arxiv.org/abs/1709.02861
Autor:
Wade, G. A., Neiner, C., Alecian, E., Grunhut, J. H., Petit, V., de Batz, B., Bohlender, D. A., Cohen, D. H., Henrichs, H. F., Kochukhov, O., Landstreet, J. D., Manset, N., Martins, F., Mathis, S., Oksala, M. E., Owocki, S. P., Rivinius, Th., Shultz, M. E., Sundqvist, J. O., Townsend, R. H. D., ud-Doula, A., Bouret, J. -C., Braithwaite, J., Briquet, M., Carciofi, A. C., David-Uraz, A., Folsom, C. P., Fullerton, A. W., Leroy, B., Marcolino, W. L. F., Moffat, A. F. J., Nazé, Y., Aurière, M., Bagnulo, S., Bailey, J. D., Barbá, R. H., Blazère, A., Böhm, T., Catala, C., Donati, J. -F., Ferrario, L., Harrington, D., Howarth, I. D., Ignace, R., Kaper, L., Lüftinger, T., Prinja, R., Vink, J. S., Weiss, W. W., Yakunin, I.
Publikováno v:
MNRAS, 456, 2-22 (2016)
The MiMeS project is a large-scale, high resolution, sensitive spectropolarimetric investigation of the magnetic properties of O and early B type stars. Initiated in 2008 and completed in 2013, the project was supported by 3 Large Program allocations
Externí odkaz:
http://arxiv.org/abs/1511.08425
We model the full-Stokes spectrum of the brown dwarf LSR J1835+3259 in the bands of the diatomic molecules CrH, TiO, and FeH in order to infer its magnetic properties. The models are then compared to the observational data obtained with the Low Resol
Externí odkaz:
http://arxiv.org/abs/1503.06964
We model the spectra of two brown dwarfs observed with the low resolution spectropolarimeter LRIS (Keck observatory) during several rotational phases in order to infer their magnetic properties. The spectra modeled include the intensity signal (Stoke
Externí odkaz:
http://arxiv.org/abs/1309.4617
Context: The technique of matching synthetic spectra computed with theoretical stellar atmosphere models to the observations is widely used in deriving fundamental parameters of massive stars. When applied to binaries, however, these models generally
Externí odkaz:
http://arxiv.org/abs/1307.1970
Telescopes often modify the input polarization of a source so that the measured circular or linear output state of the optical signal can be signficantly different from the input. This mixing, or polarization "cross-talk", is defined by the optical s
Externí odkaz:
http://arxiv.org/abs/1105.2615
A number of binary systems present evidence of enhanced activity around periastron passage, suggesting a connection between tidal interactions and these periastron effects. The aim of this investigation is to study the time-dependent response of a st
Externí odkaz:
http://arxiv.org/abs/1102.4301
Sensitive measurements of the linearly polarized spectra of stars can be used to deduce geometric properties of their otherwise unresolved circumstellar environments. This paper describes some of the evidence for optical pumping and absorptive linear
Externí odkaz:
http://arxiv.org/abs/1010.0705