322 research outputs found
Beam Shape and Halo Monitor Study
The Beam Shape and Halo Monitor, designed by Masaki Hori, is the main diagnostic tool for the 3 MeV test stand scheduled in 2008. This detector will be able to measure the transverse halo generated in the RFQ and the Chopper-line and to detect and measure the longitudinal halo composed of the incompletely chopped bunches. Its principle of functioning is the following: H- ions hit a carbon foil and generate secondary electrons with the same spatial distribution than the incoming beam and a current depending on an emission coefficient given by the carbon foil. These electrons are accelerated towards a phosphor screen by an electric field applied between accelerating grids. Once the electrons reach the phosphor screen, they generate light which is transmitted to a CCD camera via optic fibers [1]. It is expected to give a time resolution of 1-2ns and a spatial resolution of 1mm. The first test of the BSHM done with a Laser has shown a spatial resolution bigger than 1cm and the time resolution bigger than 2ns[2]. The purpose of this study is to understand what are the processes which deteriorate the resolution and to show the benefits brought by adding a pre-accelerating grid in the detector
End-to end simulations of LINAC4
Linac4 is a new H- linear accelerator presently studied at CERN. This machine consists of normal-conducting structures operating at 352.2 MHz and 704.4 MHz re-using the RF equipment from the decommissioned LEP collider. It consists of a 95 keV H- source, a 352 MHz RFQ bringing the energy the energy to 3 MeV, a Chopper line, a 352 MHz Drift Tube Linac bringing the energy to 40 MeV, a 352 MHz Coupled Cavity Drift Tube Linac bringing the energy to 90 MeV and a 704 MHz Side Coupled Linac bringing the energy to 160 MeV. Each section is designed and optimized as stand-alone machines for a good transmission and minimum possible emittance growth. End-to-end simulations starting from the RFQ have been carried out in order to validate and compare the multiparticle simulation codes PATH Manager and TRACEWIN used for beam dynamics calculations as well as to perform a global optimization of the structures in the context of a complex machine
The Ionization of the Local Interstellar Medium, as Revealed by FUSE Observations of N, O and Ar toward White Dwarf Stars
FUSE spectra of the white dwarf stars G191-B2B, GD 394, WD 2211-495 and WD
2331-475 cover the absorption features out of the ground electronic states of N
I, N II, N III, O I and Ar I in the far ultraviolet, providing new insights on
the origin of the partial ionization of the Local Interstellar Medium (LISM),
and for the case of G191-B2B, the interstellar cloud that immediately surrounds
the solar system. Toward these targets the interstellar abundances of Ar I, and
sometimes N I, are significantly below their cosmic abundances relative to H I.
In the diffuse interstellar medium, these elements are not likely to be
depleted onto dust grains. Generally, we expect that Ar should be more strongly
ionized than H (and also O and N whose ionizations are coupled to that of H via
charge exchange reactions) because the cross section for the photoionization of
Ar I is very high. Our finding that Ar I/H I is low may help to explain the
surprisingly high ionization of He in the LISM found by other investigators.
Our result favors the interpretation that the ionization of the local medium is
maintained by a strong EUV flux from nearby stars and hot gases, rather than an
incomplete recovery from a past, more highly ionized condition.Comment: 13 pages, 2 figures. To appear in a special issue of the
Astrophysical Journal Letters devoted to the first scientific results from
the FUSE missio
Updated layout of the LINAC4 transfer line to the PS Booster (Green Field Option)
At the time of defining the site of Linac4 and its integration in the complex of existing infrastructure at CERN (together with the plans for a future Superconducting Proton Linac), a series of radiation protection issues emerged that have since prompted a revision of the Linac4 to PSB transfer line layout, as was described in the document ABùNoteù2007ù037. For radiological safety reasons the distance between the planned SPL tunnel and the basement of building 513 had to be increased, and this led to the decision to lower the Linac4 machine by 2.5m. A vertical ramp was consequently introduced in the transfer line to raise the beam at the same level of LINAC2/PSB for connection to the existing transfer line. A series of error study runs has been carried out on the modified layout to have an estimate of the losses induced by quadrupole alignment and field errors. The two worst cases of each error family have been used as case studies to test the efficiency of possible steering strategies in minimizing beam losses and machine activation. The new layout and beam dynamics issues plus the results of the error and steering studies are discussed in this note
Deuterium Toward WD1634-573: Results from the Far Ultraviolet Spectroscopic Explorer (FUSE) Mission
We use Far Ultraviolet Spectrocopic Explorer (FUSE) observations to study
interstellar absorption along the line of sight to the white dwarf WD1634-573
(d=37.1+/-2.6 pc). Combining our measurement of D I with a measurement of H I
from Extreme Ultraviolet Explorer data, we find a D/H ratio toward WD1634-573
of D/H=(1.6+/-0.5)e-5. In contrast, multiplying our measurements of D I/O
I=0.035+/-0.006 and D I/N I=0.27+/-0.05 with published mean Galactic ISM gas
phase O/H and N/H ratios yields D/H(O)=(1.2+/-0.2)e-5 and
D/H(N)=(2.0+/-0.4)e-5, respectively. Note that all uncertainties quoted above
are 2 sigma. The inconsistency between D/H(O) and D/H(N) suggests that either
the O I/H I and/or the N I/H I ratio toward WD1634-573 must be different from
the previously measured average ISM O/H and N/H values. The computation of
D/H(N) from D I/N I is more suspect, since the relative N and H ionization
states could conceivably vary within the LISM, while the O and H ionization
states will be more tightly coupled by charge exchange.Comment: 23 pages, 5 figures; AASTEX v5.0 plus EPSF extensions in mkfig.sty;
accepted by ApJ Supplemen
Effect of the heliospheric interface on the distribution of interstellar hydrogen atom inside the heliosphere
This paper deals with the modeling of the interstellar hydrogen atoms (H
atoms) distribution in the heliosphere. We study influence of the heliospheric
interface, that is the region of the interaction between solar wind and local
interstellar medium, on the distribution of the hydrogen atoms in vicinity of
the Sun. The distribution of H atoms obtained in the frame of the
self-consistent kinetic-gasdynamic model of the heliospheric interface is
compared with a simplified model which assumes Maxwellian distribution of H
atoms at the termination shock and is called often as 'hot' model. This
comparison shows that the distribution of H atoms is significantly affected by
the heliospheric interface not only at large heliocentric distances, but also
in vicinity of the Sun at 1-5 AU. Hence, for analysis of experimental data
connected with direct or undirect measurements of the interstellar atoms one
necessarily needs to take into account effects of the heliospheric interface.
In this paper we propose a new model that is relatively simple but takes into
account all major effects of the heliospheric interface. This model can be
applied for analysis of backscattered Ly-alpha radiation data obtained on board
of different spacecraft.Comment: published in Astronomy Letter
Loss Control and Steering Strategy for the CERN LINAC4
A series of runs with the aim of defining alignment and gradient tolerances for the quadrupoles have been performed on the LINAC4 reference layout. The results, the implication on the machine layout and the correction schemes are reported in this paper
The Structure of the Local Interstellar Medium V: Electron Densities
We present a comprehensive survey of CII* absorption detections toward stars
within 100 pc in order to measure the distribution of electron densities
present in the local interstellar medium (LISM). Using high spectral resolution
observations of nearby stars obtained by GHRS and STIS onboard the Hubble Space
Telescope, we identify 13 sight lines with 23 individual CII* absorption
components, which provide electron density measurements, the vast majority of
which are new. We employ several strategies to determine more accurate CII
column densities from the saturated CII resonance line, including, constraints
of the line width from the optically thin CII* line, constraints from
independent temperature measurements of the LISM gas based on line widths of
other ions, and third, using measured SII column densities as a proxy for CII
column densities. The sample of electron densities appears consistent with a
log-normal distribution and an unweighted mean value of n_e(CII_SII) =
0.11^+0.10_-0.05 cm^-3. Seven individual sight lines probe the Local
Interstellar Cloud (LIC), and all present a similar value for the electron
density, with a weighted mean of n_e(LIC) = 0.12 +/- 0.04 cm^-3. The Hyades
Cloud, a decelerated cloud at the leading edge of the platoon of LISM clouds,
has a significantly higher electron density than the LIC. Observed toward
G191-B2B, the high electron density may be caused by the lack of shielding from
such a strong radiation source. Given some simple assumptions, the range of
observed electron densities translates into a range of thermal pressures, P/k =
3300^+5500_-1900 K cm^-3. This work greatly expands the number of electron
density measurements and provides important constraints on the ionization,
abundance, and evolutionary models of the local interstellar medium. (abridged)Comment: 41 pages, 9 figures; Accepted for publication in Ap
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