1,725,116 research outputs found
Taylor, R, 2/4104
No full textThis record was harvested from a previous catalogue system and will be withdrawn in 2025. Information in this record may be superseded or incomplete. Visit this record in UMA's new catalogue at: https://archives.library.unimelb.edu.au/nodes/view/428368Surname: Taylor. Given Name(s) or Initials: R. Military Service Number or Last Known Location: 2/4104. Prisoner of War Enquiry Card Index Number: K.230. Division Enquiry: NSW. Rank: PTE. Unit: [No Unit]327124
Item: [2016.0049.60630] "Taylor, R, 2/4104
Astronomische Nachrichten, nos 4081-4104
No full textAstronomische Nachrichten, nos 4081-4104. In: Bulletin astronomique, tome 24, 1907. pp. 367-377
C.N.R. steam engine #4104, unknown location
No full textHandwritten on back: "CNR Engine #4104 Double Header Freight Train"
Block Card 4104 Nebraska Avenue
No full textThis image was produced by the Auditor's Office in Lucas County, Ohio for tax assessment purposes. Associated dates are approximate. Descriptive terms related to this photograph include: Dwelling | Mount Vernon Subdivision (Toledo, Ohio) | Inverness Area (Toledo, Ohio) | 4104 Nebraska Avenue (Toledo, Ohio) | Cape Cod Styl
BCP 4104 PUBLIC SECTOR MANAGEMENT EXAM MRUC APRIL 2016
No full textBCP 4104 PUBLIC SECTOR MANAGEMENT EXAM MRUC APRIL 201
An H2O maser in the infrared source IRAS 20126+4104
Get PDFResults of monitoring of H2O maser in the infrared source IRAS 20126+4104, which is associated with a cool molecular cloud, are presented. The observations were carried out on the 22-meter radio telescope of the Pushchino Radio Astronomy Observatory (Russia) between June 1991 and January 2006. The spectrum of the H2O maser emission extends from −16.7 to 4.8 km/s and splits into separate groups of emission features. Cyclic variations of the integrated maser flux with a period from 3.4 to 5.5 years were detected, together with strong flares of up to 220 Jy in individual emission features. It is shown that large linewidths in periods of high maser activity are due to small-scale turbulent motions of the material. An expanding envelope around a young star is accepted as a model for the source. The protostar has a small peculiar velocity with respect to the molecular cloud (∼2 km/s). Individual emission features form organized structures, including multi-link chains
Block Card 4104 Commonwealth Avenue
No full textThis image was produced by the Auditor's Office in Lucas County, Ohio for tax assessment purposes. Associated dates are approximate. Descriptive terms related to this photograph include: dwelling | 4104 Commonwealth Avenue (Toledo, Ohio) | Colonial Revival Style | Commonwealth Addition (Toledo, Ohio) | Willys Park area (Toledo, Ohio) | West Toledo (Toledo, Ohio
Block Card 4104 Lewis Avenue
No full textThis image was produced by the Auditor's Office in Lucas County, Ohio for tax assessment purposes. Associated dates are approximate. Descriptive terms related to this photograph include: automobile repair shops | barns | 4104 Lewis Avenue (Toledo, Ohio) | Willys Park Area (Toledo, Ohio) | West Toledo Area (Toledo, Ohio
Sub-arcsecond resolution radio continuum observations of IRAS 20126+4104
No full textContext.The detailed physical processes that lead to the formation of massive
stars are still unknown. Observations that probe linear scales as small
as AU are necessary for improving our understanding in this area.
Aims.
We present high angular-resolution and
high-sensitivity multi-frequency radio observations of the deeply
embedded
massive protostar located in the IRAS 20126+4104 core
region, with the aim of investigating the nature of the radio continuum
emission from the deeply embedded massive protostar.
Methods.
The observations were performed with the Very Large Array in several
continuum bands with wavelengths between 20 and 0.7 cm in the
A and/or B configurations.
Results.
At 3.6 cm we resolve the emission of the IRAS 20126+4104 core into 3 components.
The emission from the two northern sources is consistent with free-free
emission from ionized gas with a density gradient. Most likely the
ionization is caused by UV radiation from the cooling region of a
shock;
i.e. the ionization is caused by the jet driven by the IRAS 20126+4104 protostar.
The morphology and measured flux densities of the southern source is
consistent with emission from an optically thin jet, most likely also
due to shock ionization.
A simple radiative transfer model shows that the
spectral energy distribution of IRAS 20126+4104 is consistent with an accretion
disk embedded in a spherical halo.
We also report the discovery of a highly variable radio source near
the IRAS 20126+4104 core, which is most likely gyrosynchotron emission
from a low-mass pre-main sequence star
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