scholarly journals Time-Resolved High-Resolution Spectroscopy of roAp Stars

2002 ◽  
Vol 185 ◽  
pp. 284-287
Author(s):  
O. Kochukhov ◽  
T. Ryabchikova
Keyword(s):  
Rare Earth ◽  
High Resolution ◽  
Detailed Analysis ◽  
High Resolution Spectroscopy ◽  
Spectral Features ◽  
Line Profiles ◽  
Time Resolved ◽  
Spectroscopic Monitoring ◽  
Rotational Modulation ◽  
Very High

AbstractWe report results of Spectroscopic monitoring of the roAp stars γ Equ, α Cir and HR 3831 with the ESO 3.6-meter telescope. Series of very high-resolution and high S/N spectra allowed to resolve changes of line profiles due to the pulsations. We found that pulsational behaviour of all three roAp stars is dominated by the variations of the doubly ionized rare-earth lines. Detailed analysis of the pulsational changes of Nd III and Pr III spectral features allowed us to identify the pulsational mode of γ Equ and to study rotational modulation of the pulsational pattern in the spectra of α Cir and HR 3831.

scholarly journals The Voyage of Metals in the Universe from Cosmological to Planetary Scales: the need for a Very High-Resolution, High Throughput Soft X-ray Spectrometer

2021 ◽  
Author(s):  
F. Nicastro ◽  
J. Kaastra ◽  
C. Argiroffi ◽  
E. Behar ◽  
S. Bianchi ◽  
...  
Keyword(s):  
Chemical Composition ◽  
High Resolution ◽  
Deep Understanding ◽  
High Resolution Spectroscopy ◽  
X Ray ◽  
Viable Solution ◽  
Surrounding Space ◽  
Nuclear Processes ◽  
The Universe ◽  
Very High

AbstractMetals form an essential part of the Universe at all scales. Without metals we would not exist, and the Universe would look completely different. Metals are primarily produced via nuclear processes in stars, and spread out through winds or explosions, which pollute the surrounding space. The wanderings of metals in-and-out of astronomical objects are crucial in determining their own evolution and thus that of the Universe as a whole. Detecting metals and assessing their relative and absolute abundances and energetics can thus be used to trace the evolution of these cosmic components. The scope of this paper is to highlight the most important open astrophysical problems that will be central in the next decades and for which a deep understanding of the Universe’s wandering metals, their physical and kinematical states, and their chemical composition represents the only viable solution. The majority of these studies can only be efficiently performed through High Resolution Spectroscopy in the soft X-ray band.

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.

scholarly journals New Progress in Mode Detection and Identification in δ Scuti Stars by the Analysis of Line Profile Variations

2000 ◽  
Vol 176 ◽  
pp. 463-464
Author(s):  
L. Mantegazza ◽  
E. Poretti ◽  
M. Bossi ◽  
N. S. Nuñez ◽  
A. Sacchi ◽  
...  
Keyword(s):  
High Resolution ◽  
Line Profile ◽  
High Resolution Spectroscopy ◽  
Line Profiles ◽  
Powerful Technique ◽  
Mode Detection ◽  
Detection And Identification ◽  
Scuti Stars ◽  
Δ Scuti Stars ◽  
Nonradial Pulsation

Abstractδ Sct stars are among the most promising targets to perform ground-based asteroseismology. High resolution spectroscopy offers us a powerful technique to identify radial and nonradial pulsation modes, since we can easily detect oscillations and travelling features in the line profiles.

Orographic clouds in north Victoria Land from AVHRR images

Polar Record ◽  
1996 ◽  
Vol 32 (183) ◽  
pp. 317-324 ◽  
Author(s):  
Giuseppe Zibordi ◽  
Massimo Frezzotti
Keyword(s):  
High Resolution ◽  
Satellite Imagery ◽  
Meteorological Data ◽  
Spectral Features ◽  
Katabatic Winds ◽  
Victoria Land ◽  
Avhrr Data ◽  
Orographic Clouds ◽  
Temporal Occurrence ◽  
Very High

ABSTRACTOrographic clouds over north Victoria Land, East Antarctica, have been observed in Advanced Very High Resolution Radiometer (AVHRR) satellite imagery. These occasional clouds are discussed through analysis of their spectral features in AVHRR data. Temporal occurrence, spatial extension, and direction of the clouds are also discussed in relation to meteorological data for two periods characterised by katabatic winds, in December 1992 and January 1993.

scholarly journals Very high-resolution spectroscopy for extremely large telescopes using pupil slicing and adaptive optics

2007 ◽  
Vol 15 (5) ◽  
pp. 1983 ◽  
Author(s):  
Jacques M. Beckers ◽  
Torben E. Andersen ◽  
Mette Owner-Petersen
Keyword(s):  
High Resolution ◽  
Adaptive Optics ◽  
High Resolution Spectroscopy ◽  
Large Telescopes ◽  
Very High

Very high-resolution spectroscopy: the ESPRESSO optical design

2012 ◽  
Author(s):  
P. Spanò ◽  
B. Delabre ◽  
H. Dekker ◽  
F. Pepe ◽  
F. M. Zerbi ◽  
...  
Keyword(s):  
High Resolution ◽  
Optical Design ◽  
High Resolution Spectroscopy ◽  
Very High

scholarly journals High Resolution Spectroscopy of CF3Br by Diode Laser in the Frequency Range 1070–1090 cm−1

1988 ◽  
Vol 8 (1) ◽  
pp. 61-78 ◽  
Author(s):  
R. de Bekker ◽  
M. Ebben ◽  
M. Snels ◽  
S. Stolte
Keyword(s):  
High Resolution ◽  
Diode Laser ◽  
Absorption Spectra ◽  
High Resolution Spectroscopy ◽  
Ir Absorption ◽  
Spectral Features ◽  
Frequency Range ◽  
Molecular Constants ◽  
Ir Absorption Spectra ◽  
Better Than

The IR absorption spectra of gaseous CF3Br expanded in a molecular jet have been recorded with a linewidth of about 0.002 cm−1. The rotational K-structure of the ν1 fundamental has been resolved and the molecular constants ΔB and ΔA have been determined with an accuracy better than 5 x 10−6 cm−1. Spectral features belonging to the ν6- and ν3-hotbands have been identified. For CF3B79r (CF3B81r) improved values of the vibrational origins for the fundamental ν1 = 1084.768(2) cm−1 (1084.520(2) cm−1) and for its hotbands ν3+ν1←ν3 = 1081.709(80) cm−1 (1081.065(40) cm−1) and ν6+ν1←ν6 = 1083.533(4) cm-1 (1083.288(4) cm-1) have been determined.

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