An infrared diagnostic for magnetism in hot stars
Identifikátory výsledku
Kód výsledku v IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F15%3A00450614" target="_blank" >RIV/67985815:_____/15:00450614 - isvavai.cz</a>
Výsledek na webu
<a href="http://dx.doi.org/10.1051/0004-6361/201525987" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201525987</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1051/0004-6361/201525987" target="_blank" >10.1051/0004-6361/201525987</a>
Alternativní jazyky
Jazyk výsledku
angličtina
Název v původním jazyce
An infrared diagnostic for magnetism in hot stars
Popis výsledku v původním jazyce
Magnetospheric observational proxies are used for indirect detection of magnetic fields in hot stars in the X-ray, UV, optical, and radio wavelength ranges. To determine the viability of infrared (IR) hydrogen recombination lines as a magnetic diagnostic for these stars, we have obtained low-resolution (R similar to 1200), near-IR spectra of the known magnetic B2V stars HR 5907 and HR 7355, taken with the Ohio State Infrared Imager/Spectrometer (OSIRIS) attached to the 4.1 m Southern Astrophysical Research (SOAR) Telescope. Both stars show definite variable emission features in IR hydrogen lines of the Brackett series, with similar properties as those found in optical spectra, including the derived location of the detected magnetospheric plasma. These features also have the added advantage of a lowered contribution of stellar flux at these wavelengths, making circumstellar material more easily detectable. IR diagnostics will be useful for the future study of magnetic hot stars, to detect and analyze lower-density environments, and to detect magnetic candidates in areas obscured from UV and optical observations, increasing the number of known magnetic stars to determine basic formation properties and investigate the origin of their magnetic fields.
Název v anglickém jazyce
An infrared diagnostic for magnetism in hot stars
Popis výsledku anglicky
Magnetospheric observational proxies are used for indirect detection of magnetic fields in hot stars in the X-ray, UV, optical, and radio wavelength ranges. To determine the viability of infrared (IR) hydrogen recombination lines as a magnetic diagnostic for these stars, we have obtained low-resolution (R similar to 1200), near-IR spectra of the known magnetic B2V stars HR 5907 and HR 7355, taken with the Ohio State Infrared Imager/Spectrometer (OSIRIS) attached to the 4.1 m Southern Astrophysical Research (SOAR) Telescope. Both stars show definite variable emission features in IR hydrogen lines of the Brackett series, with similar properties as those found in optical spectra, including the derived location of the detected magnetospheric plasma. These features also have the added advantage of a lowered contribution of stellar flux at these wavelengths, making circumstellar material more easily detectable. IR diagnostics will be useful for the future study of magnetic hot stars, to detect and analyze lower-density environments, and to detect magnetic candidates in areas obscured from UV and optical observations, increasing the number of known magnetic stars to determine basic formation properties and investigate the origin of their magnetic fields.
Klasifikace
Druh
J<sub>imp</sub> - Článek v periodiku v databázi Web of Science
CEP obor
—
OECD FORD obor
10308 - Astronomy (including astrophysics,space science)
Návaznosti výsledku
Projekt
<a href="/cs/project/GA14-21373S" target="_blank" >GA14-21373S: Odhalení historie ztráty hmoty vyvinutých masivních hvězd</a><br>
Návaznosti
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Ostatní
Rok uplatnění
2015
Kód důvěrnosti údajů
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Údaje specifické pro druh výsledku
Název periodika
Astronomy & Astrophysics
ISSN
1432-0746
e-ISSN
—
Svazek periodika
578
Číslo periodika v rámci svazku
June
Stát vydavatele periodika
FR - Francouzská republika
Počet stran výsledku
4
Strana od-do
"A112/1"-"A112/4"
Kód UT WoS článku
000357502600124
EID výsledku v databázi Scopus
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