53 research outputs found
High Velocity Rain: The Terminal Velocity of Model of Galactic Infall
A model is proposed for determining the distances to falling interstellar
clouds in the galactic halo by measuring the cloud velocity and column density
and assuming a model for the vertical density distribution of the Galactic
interstellar medium. It is shown that falling clouds with may be decelerated to a terminal velocity which increases with
increasing height above the Galactic plane. This terminal velocity model
correctly predicts the distance to high velocity cloud Complex M and several
other interstellar structures of previously determined distance. It is
demonstrated how interstellar absorption spectra alone may be used to predict
the distances of the clouds producing the absorption. If the distances to the
clouds are already known, we demonstrate how the model may be used to determine
the vertical density structure of the ISM. The derived density distribution is
consistent with the expected density distribution of the warm ionized medium,
characterized by Reynolds. There is also evidence that for
one or more of the following occurs: (1) the neutral fraction of the cloud
decreases to , (2) the density drops off faster than
characterized by Reynolds, or (3) there is a systematic decrease in drag
coefficient with increasing z.Comment: ApJ, in pres
Distances and Metallicities of High- and Intermediate-Velocity Clouds
A table is presented that summarizes published absorption line measurements
for the high- and intermediate velocity clouds (HVCs and IVCs). New values are
derived for N(HI) in the direction of observed probes, in order to arrive at
reliable abundances and abundance limits (the HI data are described in Paper
II). Distances to stellar probes are revisited and calculated consistently, in
order to derive distance brackets or limits for many of the clouds, taking care
to properly interpret non-detections. The main conclusions are the following.
1) Absolute abundances have been measured using lines of SII, NI and OI, with
the following resulting values: ~0.1 solar for one HVC (complex C), ~0.3 solar
for the Magellanic Stream, ~0.5 solar for a southern IVC, and ~ solar for two
northern IVCs (the IV Arch and LLIV Arch). Finally, approximate values in the
range 0.5-2 solar are found for three more IVCs. 2) Depletion patterns in IVCs
are like those in warm disk or halo gas. 3) Most distance limits are based on
strong UV lines of CII, SiII and MgII, a few on CaII. Distance limits for major
HVCs are >5 kpc, while distance brackets for several IVCs are in the range
0.5-2 kpc. 4) Mass limits for major IVCs are 0.5-8x10^5 M_sun, but for major
HVCs they are >10^6 M_sun. 5) The CaII/HI ratio varies by up to a factor 2-5
within a single cloud, somewhat more between clouds. 6) The NaIHI ratio varies
by a factor >10 within a cloud, and even more between clouds. Thus, CaII can be
useful for determining both lower and upper distance limits, but NaI only
yields upper limits.Comment: To appear in the "Astrophysical Journal Supplement"; 82 pages;
figures 6, 9 and 10 are in color; degraded figures (astro-ph restriction) -
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Experimental and theoretical investigation of high gradient acceleration
This report contains a technical progress summary of the research conducted under the auspices of DOE Grant No. DE-FG0291ER-40648. Experimental and Theoretical Investigations of High Gradient Acceleration.'' This grant supports three research tasks: Task A consists of the design and fabrication of a 17GHz of photocathode gun, Task B supports the testing of high gradient acceleration using a 33GHz structure, and Task C comprises theoretical investigations, both in support of the experimental tasks and on critical physics issues for the development of high energy linear colliders. This report is organized as follows. The development of an rf gun design and research progress on the picosecond laser system is summarized in Sec. 2, the status of the studies of the LBL/Haimson high gradient structure, using a 50 MW free-electron laser is summarized in Sec. 3, and theoretical research progress is described in Sec. 4. Supporting material is contained in Appendices A-G
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