Investigation of the Magnetic Field from Observations of the OH Maser in the G10.624-0.385 Star Formation Region

被引：0

作者：

Ashimbaeva, N. T. ^{[1
]}

Lekht, E. E. ^{[1
]}

Krasnov, V. V. ^{[2
]}

Tolmachev, A. M. ^{[3
]}

机构：

[1] Lomonosov Moscow State Univ, Sternberg Astron Inst, Moscow 119991, Russia

[2] Russian Acad Sci, Astro Space Ctr, PN Lebedev Phys Inst ASC LPI, Moscow 117997, Russia

[3] Russian Acad Sci, Lebedev Phys Inst, Astro Space Ctr, Pushchino Radio Astron Observ, Pushchino 142290, Russia

来源：

ASTRONOMY REPORTS | 2023年 / 67卷 / 07期

关键词：

star formation; OH masers; molecular clouds and bipolar outflows; polarization; magnetic field; FORMING REGIONS; OB CLUSTERS; EMISSION; EVOLUTION; W31;

D O I：

10.1134/S1063772923070016

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The results of a study of the variability of maser emission in OH lines in the 18 cm range in the G10.624-0.385 star formation region from monitoring data performed at the Large Radio Telescope in Nancay (France) in 2008-2023 are presented. It is obtained that for a Zeeman pair in line 1667 MHz splitting (about 1.96 km/s) and, consequently, the magnitude of the longitudinal magnetic field have been stable for more than 25 years. In the satellite lines of 1612 and 1720 MHz, broadband absorption and emission are observed, respectively. The mirrored profiles of the OH 1612 and 1720 MHz satellite lines indicate that the levels of the corresponding transitions are pumped by IR radiation from a source immersed in a magnetized molecular cloud around the OH maser. Spatial identification of features in both main lines is carried out. It is found that the transverse magnetic field is directed mainly along some organized structure in the form of an arc.

引用

页码：707 / 718

页数：12

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