scholarly journals Time-resolved spectroscopic observations of an M-dwarf flare star EV Lacertae during a flare

Author(s):  
Satoshi Honda ◽  
Yuta Notsu ◽  
Kosuke Namekata ◽  
Shota Notsu ◽  
Hiroyuki Maehara ◽  
...  
2019 ◽  
Vol 25 (S2) ◽  
pp. 826-827
Author(s):  
Brian Wingender ◽  
Emma Tong ◽  
John Emery ◽  
Laurie Gower ◽  
Roland Kröger

2004 ◽  
Vol 292 (1-4) ◽  
pp. 697-703 ◽  
Author(s):  
Inés Crespo-Chacón ◽  
David Montes ◽  
María José Fernández-Figueroa ◽  
Javier López-Santiago ◽  
David GarcÍa-Alvarez ◽  
...  

2012 ◽  
Vol 750 (2) ◽  
pp. L32 ◽  
Author(s):  
Kevin France ◽  
Jeffrey L. Linsky ◽  
Feng Tian ◽  
Cynthia S. Froning ◽  
Aki Roberge

2000 ◽  
Vol 318 (2) ◽  
pp. 440-452 ◽  
Author(s):  
Elena Mason ◽  
Warren Skidmore ◽  
Steve B. Howell ◽  
David R. Ciardi ◽  
Stuart Littlefair ◽  
...  

2010 ◽  
Vol 140 (5) ◽  
pp. 1402-1413 ◽  
Author(s):  
Eric J. Hilton ◽  
Andrew A. West ◽  
Suzanne L. Hawley ◽  
Adam F. Kowalski

1983 ◽  
Vol 71 ◽  
pp. 207-221
Author(s):  
Simon P. Worden

As for solar flares, one of the most physically revealing types of data for M-dwarf flares are high-resolution, time-resolved spectra. Due to the intrinsically faint nature of the M-dwarf stars, spectroscopic data has tended to be of low spectral (˜ 5 Ǻ) and temporal (˜ 5 min) resolution. However, with the development of image intensified spectrographs and fast, efficient digital detectors, the last several years have seen the successful acquisition of both high time and spectral resolution M-dwarf flare spectra. Recent programs have also been successfully conducted using the International Ultraviolet Explorer (IUE) satellite to obtain UV and EUV spectra of M-dwarf flares. These data reveal that dwarf M star flares are remarkably similar to solar flares in all aspects of their spectroscopic phenomenology.


2012 ◽  
Author(s):  
Kosuke Kurosawa ◽  
T. Kadono ◽  
S. Sugita ◽  
K. Shigemori ◽  
Yoichiro Hironaka ◽  
...  

1983 ◽  
Vol 71 ◽  
pp. 157-174
Author(s):  
Patrick B. Byrne

This review discusses optical observations of flares and the results gleaned from these. Excellent reviews of flare activity have been published in the past and one might mention in particular Kunkel (1975), Gershberg (1978) and Gurzadyan (1980). In general these have been more broadly based than the present review incorporating other aspects of flare stars e.g. BY Dra variability, spectroscopic observations, etc. Since these other aspects of flare star behaviour are being covered elsewhere in this volume we will confine ourselves exclusively to optical photometry of the flare phenomenon itself. We will also confine ourselves to the solar-neighbourhood flare stars (i.e. the UV Ceti stars) since other contributors will discuss the T-Taurl, RS CVn, BY Dra and other flaring objects.


Nanomaterials ◽  
2021 ◽  
Vol 11 (10) ◽  
pp. 2767
Author(s):  
Yu Liu ◽  
Ziwen Zhou ◽  
Shaojian Zhang ◽  
Enming Zhao ◽  
Jing Ren ◽  
...  

To date, the mechanisms of Er3+ upconversion luminescence via 980 and 1530 nm excitation have been extensively investigated; however, based on discussions, they either suffer from the lack of convincing evidence or require elaborated and time-consuming numerical simulations. In this work, the steady-state and time-resolved upconversion luminescence data of Er3+-doped NaYF4 were measured; we therefore investigated the upconversion mechanisms of Er3+ on the basis of the spectroscopic observations and the simplified rate equation modeling. This work provides a relatively simple strategy to reveal the UCL mechanisms of Er3+ upon excitation with various wavelengths, which may also be used in other lanthanide ion-doped systems.


2000 ◽  
Vol 318 (2) ◽  
pp. 429-439 ◽  
Author(s):  
Warren Skidmore ◽  
Elena Mason ◽  
Steve B. Howell ◽  
David R. Ciardi ◽  
Stuart Littlefair ◽  
...  

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