The maser is based on the principle of stimulated emission proposed by Albert Einstein in 1917. For their research in this field Townes, Basov and Prokhorov were awarded the Nobel Prize in Physics in 1964. Schawlow to describe the principle of the optical maser, or laser, which Theodore H. The device used stimulated emission in a stream of energized ammonia molecules to produce amplification of microwaves at a frequency of 24 gigahertz. Zeiger built the first maser at Columbia University in 1953. They subsequently published their results in October 1954. Our results strongly support models that predict IR radiative pumping for the 6.7 GHz CH 3OH masers.Theoretically, reflecting principles previously discussed by Joseph Weber at the June 1952 conference of the Institute of Radio Engineers, the principle of the maser was described by Nikolay Basov and Alexander Prokhorov from Lebedev Institute of Physics at an All-Union Conference on Radio-Spectroscopy held by USSR Academy of Sciences in May 1952. Both the maser flare and the extraordinarily large extent of the maser structure can be a natural consequence of the burst in the accretion luminosity of the high-mass YSO. In particular, the outburst peak emission originates from a remarkably extended (0.̋2–0.̋3) maser plateau at a radial distance of 500–1000 AU from the source.Ĭonclusions. Compared to the pre-burst phase, flaring 6.7 GHz masers emit across a different V LSR range that is more strongly redshifted, and the emission extends over a larger area at larger separation from the high-mass YSO. The main pre-burst maser cluster is no longer detected during the burst. Since most maser centers operate in the unsaturated regime, a change by a relatively small factor ( ≈5) in the flux of pumping photons has produced an exponential growth in the maser intensity. The accretion burst and the subsequent increase in IR luminosity are very likely the origin of the 6.7 GHz maser flare. Jansky Very Large Array (JVLA) and the European VLBI Network (EVN), we performed observations of the 6.7 GHz masers (covering a range in angular resolution from a few milliarcseconds to ≈1 ′′) during the burst phase and compared these observations with pre-burst measurements at similar spatial scales. Our goal is to study the change in the properties of the 6.7 GHz masers between the pre- and outburst phases, and investigate the connection between the maser and the accretion burst. Recently, substantial flaring in the 6.7 GHz methanol maser line has been observed toward the high-mass young stellar object (YSO) S255 NIRS 3, where an accretion burst was also detected in the IR. Fermi 5, 50125 Firenze, ItalyĮ-mail: Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germanyģ Department of Astrophysics/IMAPP, Radboud University, PO Box 9010, 6500 GL Nijmegen, The NetherlandsĤ Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Irelandĥ Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, GermanyĪims. Kraus 2ġ INAF, Osservatorio Astrofisico di Arcetri, Largo E. Astronomical objects: linking to databases.Including author names using non-Roman alphabets. Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes
0 Comments
Leave a Reply. |
AuthorWrite something about yourself. No need to be fancy, just an overview. ArchivesCategories |