Resolving the Circumstellar Environment of the Galactic B[e] Supergiant Star MWC 137. II. Nebular Kinematics and Stellar Variability

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F21%3A00548198" target="_blank" >RIV/67985815:_____/21:00548198 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.3847/1538-3881/ac1355" target="_blank" >https://doi.org/10.3847/1538-3881/ac1355</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-3881/ac1355" target="_blank" >10.3847/1538-3881/ac1355</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Resolving the Circumstellar Environment of the Galactic B[e] Supergiant Star MWC 137. II. Nebular Kinematics and Stellar Variability

Popis výsledku v původním jazyce

The Galactic B[e] supergiant MWC137 is surrounded by a large-scale optical nebula. To shed light on the physical conditions and kinematics of the nebula, we analyze the optical forbidden emission lines [N II] lambda lambda 6548,6583 and [S II] lambda lambda 6716,6731 in long-slit spectra taken with ALFOSC at the Nordic Optical Telescope. The radial velocities display a complex behavior but, in general, the northern nebular features are predominantly approaching while the southern ones are mostly receding. The electron density shows strong variations across the nebula with values spreading from about zero to similar to 800 cm(-3). Higher densities are found closer to MWC137 and in regions of intense emission, whereas in regions with high radial velocities the density decreases significantly. We also observe the entire nebula in the two [S II] lines with the scanning Fabry-Perot interferometer attached to the 6 m telescope of the Special Astrophysical Observatory. These data reveal a new bow-shaped feature at P.A. = 225 degrees-245 degrees and a distance 80 '' from MWC137. A new H alpha image has been taken with the Danish 1.54 m telescope on La Silla. No expansion or changes in the nebular morphology appear within 18.1 yr. We derive a mass of 37(-5)(+9) M-circle dot. and an age of 4.7 +/- 0.8 Myr for MWC137. Furthermore, we detect a period of 1.93 d in the time series photometry collected with the TESS satellite, which could suggest stellar pulsations. Other, low-frequency variability is seen as well. Whether these signals are caused by internal gravity waves in the early-type star or by variability in the wind and circumstellar matter currently cannot be distinguished.

Název v anglickém jazyce

Resolving the Circumstellar Environment of the Galactic B[e] Supergiant Star MWC 137. II. Nebular Kinematics and Stellar Variability

Popis výsledku anglicky

The Galactic B[e] supergiant MWC137 is surrounded by a large-scale optical nebula. To shed light on the physical conditions and kinematics of the nebula, we analyze the optical forbidden emission lines [N II] lambda lambda 6548,6583 and [S II] lambda lambda 6716,6731 in long-slit spectra taken with ALFOSC at the Nordic Optical Telescope. The radial velocities display a complex behavior but, in general, the northern nebular features are predominantly approaching while the southern ones are mostly receding. The electron density shows strong variations across the nebula with values spreading from about zero to similar to 800 cm(-3). Higher densities are found closer to MWC137 and in regions of intense emission, whereas in regions with high radial velocities the density decreases significantly. We also observe the entire nebula in the two [S II] lines with the scanning Fabry-Perot interferometer attached to the 6 m telescope of the Special Astrophysical Observatory. These data reveal a new bow-shaped feature at P.A. = 225 degrees-245 degrees and a distance 80 '' from MWC137. A new H alpha image has been taken with the Danish 1.54 m telescope on La Silla. No expansion or changes in the nebular morphology appear within 18.1 yr. We derive a mass of 37(-5)(+9) M-circle dot. and an age of 4.7 +/- 0.8 Myr for MWC137. Furthermore, we detect a period of 1.93 d in the time series photometry collected with the TESS satellite, which could suggest stellar pulsations. Other, low-frequency variability is seen as well. Whether these signals are caused by internal gravity waves in the early-type star or by variability in the wind and circumstellar matter currently cannot be distinguished.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA20-00150S" target="_blank" >GA20-00150S: Struktura a vývoj hvězdných výtrysků</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2021

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomical Journal

ISSN

0004-6256

e-ISSN

1538-3881

Svazek periodika

162

Číslo periodika v rámci svazku

4

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

14

Strana od-do

150

Kód UT WoS článku

000697649300001

EID výsledku v databázi Scopus

2-s2.0-85116376078