Observations of Maser Emission in the Star-Forming Region G43.8-0.1. II. H2O Maser Emission at 1.35 cm

被引：2

作者：

Colom, P. ^{[1
]}

Ashimbaeva, N. T. ^{[2
]}

Lekht, E. E. ^{[2
]}

Pashchenko, M., I ^{[2
]}

Rudnitskii, G. M. ^{[2
]}

Krasnov, V. V. ^{[3
]}

Tolmachev, A. M. ^{[4
]}

机构：

[1] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris Meudon, F-92195 Meudon, France

[2] Lomonosov Moscow State Univ, Sternberg Astron Inst, Moscow 119992, Russia

[3] Russian Acad Sci, Lebedev Phys Inst, Moscow, Russia

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

来源：

ASTRONOMY REPORTS | 2019年 / 63卷 / 10期

关键词：

D O I：

10.1134/S0004629919100049

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The results of observations of water maser emission in the star-forming region G43.8-0.1, performed at a wavelength of 1.35 cm with the 22-m radio telescope of the Pushchino Radio Astronomy Observatory are presented. The integrated intensity of the maser emission in G43.8-0.1 varies quasi-periodically on characteristic time scales between 3.9 and 12.1 yr, possibly related to variations of the activity of the central star during its formation. Nine strong flares with maximum fluxes exceeding 3000 Jy were detected, and were identified with maser spots in high-resolution maps. It is argued that a shell model for the H2O maser in G43.8-0.1 is preferred.

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页码：814 / 829

页数：16

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