NanoVipa: a miniaturized high-resolution echelle spectrometer, for the monitoring of young stars from a 6U Cubesat

2017 ◽  
Vol 9 (4) ◽  
pp. 411-419 ◽  
Author(s):  
G. Bourdarot ◽  
E. Le Coarer ◽  
X. Bonfils ◽  
E. Alecian ◽  
P. Rabou ◽  
...  
Keyword(s):  
High Resolution ◽  
Young Stars ◽  
Echelle Spectrometer

scholarly journals High resolution spectroscopy of RY Tauri: variability of the Na D line profiles

1990 ◽  
Vol 137 ◽  
pp. 219-220
Author(s):  
P.P. Petrov
Keyword(s):  
High Resolution ◽  
Large Scale ◽  
Young Stars ◽  
High Resolution Spectroscopy ◽  
Line Profiles

Ejection and accretion of gas clouds in the vicinity of RY Tau were discovered. The existense of large scale “stellar prominences” around young stars is suggested.

Optical design for a high-resolution, 2--5-um infrared cryogenic echelle spectrometer

1990 ◽  
Author(s):  
Kenneth H. Hinkle ◽  
Stephen T. Ridgway ◽  
Frank E. Stuart
Keyword(s):  
High Resolution ◽  
Optical Design ◽  
Echelle Spectrometer

HIRES: the high-resolution echelle spectrometer on the Keck 10-m Telescope

1994 ◽  
Author(s):  
Steven S. Vogt ◽  
Steven L. Allen ◽  
Bruce C. Bigelow ◽  
L. Bresee ◽  
William E. Brown ◽  
...  
Keyword(s):  
High Resolution ◽  
Echelle Spectrometer

scholarly journals Probing the size of a magnetosphere of a young solar-like star

2008 ◽  
Vol 4 (S259) ◽  
pp. 413-414
Author(s):  
Catrina M. Hamilton ◽  
C. M. Johns-Krull ◽  
R. Mundt ◽  
W. Herbst ◽  
J. N. Winn
Keyword(s):  
Time Series ◽  
High Resolution ◽  
Binary System ◽  
Line Profile ◽  
Main Sequence ◽  
Time Series Data ◽  
Young Stars ◽  
Series Data ◽  
Accretion Flows ◽  
Magnetospheric Accretion

AbstractWe have obtained high resolution spectra of the pre-main sequence binary system KH 15D (V582 Mon) while the star is fully visible, fully occulted, and during several ingress and egress events over the course of five contiguous observing seasons. The Hα line profile is a standard probe of the magnetospheric accretion flows on young stars such as KH 15D. We use these time series data to map out the size of the magnetosphere and find that it changes size from one observing season to the next.

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