7,444 research outputs found
Evolution of an eruptive flare loop system
<p><b>Context:</b> Flares, eruptive prominences and coronal mass ejections are phenomena where magnetic reconnection plays an important role. However, the location and the rate of the reconnection, as well as the mechanisms of particle interaction with ambient and chromospheric plasma are still unclear.</p>
<p><b>Aims:</b> In order to contribute to the comprehension of the above mentioned processes we studied the evolution of the eruptive flare loop system in an active region where a flare, a prominence eruption and a CME occurred on August 24, 2002.</p>
<p><b>Methods:</b> We measured the rate of expansion of the flare loop arcade using TRACE 195 Å images and determined the rising velocity and the evolution of the low and high energy hard X-ray sources using RHESSI data. We also fitted HXR spectra and considered the radio emission at 17 and 34 GHZ.</p>
<p><b>Results:</b> We observed that the top of the eruptive flare loop system initially rises with a linear behavior and then, after 120 mn from the start of the event registered by GOES at 1–8 Å, it slows down. We also observed that the heating source (low energy X-ray) rises faster than the top of the loops at 195 Å and that the high energy X-ray emission (30–40 keV) changes in time, changing from footpoint emission at the very onset of the flare to being coincident during the flare peak with the whole flare loop arcade.</p>
<p><b>Conclusions:</b> The evolution of the loop system and of the X-ray sources allowed us to interpret this event in the framework of the Lin & Forbes model (2000), where the absolute rate of reconnection decreases when the current sheet is located at an altitude where the Alfvén speed decreases with height. We estimated that the lower limit for the altitude of the current sheet is km. Moreover, we interpreted the unusual variation of the high energy HXR emission as a manifestation of the non thermal coronal thick-target process which appears during the flare in a manner consistent with the inferred increase in coronal column density.</p>
First record of the alien pest Rhaponticum repens (Compositae) in the Iberian Peninsula
First record of the alien pest Rhaponticum repens (Compositae) in the Iberian Peninsula.- Rhaponticum repens is reported for the first time for the flora of the Iberian Peninsula. The species is native from Central Asia and has become invasive in Argentina, Canada, Europe and the USA. It was detected for the first time in abandoned fields from Vilablareix, near the city of Girona (Catalonia, Spain) and in the valley of the Vinalopó in Alicante (Valencia, Spain), where it was collected as early as in 1959 but misdentified. Molecular data, based on nrDNA region ITS, suggest that the reported populations may be closely related to plants from the United States. Due to the extremely noxious character of the species and the possible relationship of Spanish plants with the invasive American populations, some kind of monitoring is recommended.Rhaponticum repens (Compositae), una nueva planta alóctona para la Península Ibérica.- Se cita por primera vez la especie Rhaponticum repens para la flora de la Península Ibérica. Rhaponticum repens es una especie nativa de Asia central que actúa como invasora en diversos países como Argentina, Canadá o los Estados Unidos. Se ha encontrado por primera vez en campos de cultivo abandonados en el pueblo de Vilablareix, cerca de la ciudad de Girona (Cataluña, España) y en el valle del Vinalopó (Valencia, España), donde fue recolectada y mal identificada en 1959. Los datos moleculares, obtenidos a partir de la región ITS del nrDNA, sugieren que estas poblaciones podrían estar relacionadas con plantas invasoras de Estados Unidos. Debido al carácter extremadamente invasor de la especie, y a su posible origen secundario a partir de las poblaciones norteamericanas, se recomienda el seguimiento de estas poblacione
Keck Interferometer Nuller Data Reduction and On-Sky Performance
We describe the Keck Interferometer nuller theory of operation, data reduction, and on-sky performance, particularly as it applies to the nuller exozodiacal dust key science program that was carried out between 2008 February and 2009 January. We review the nuller implementation, including the detailed phasor processing involved in implementing the null-peak mode used for science data and the sequencing used for science observing. We then describe the Level 1 reduction to convert the instrument telemetry streams to raw null leakages, and the Level 2 reduction to provide calibrated null leakages. The Level 1 reduction uses conservative, primarily linear processing, implemented consistently for science and calibrator stars. The Level 2 processing is more flexible, and uses diameters for the calibrator stars measured contemporaneously with the interferometer’s K-band cophasing system in order to provide the requisite accuracy. Using the key science data set of 462 total scans, we assess the instrument performance for sensitivity and systematic error. At 2.0 Jy we achieve a photometrically-limited null leakage uncertainty of 0.25% rms per 10 minutes of integration time in our broadband channel. From analysis of the Level 2 reductions, we estimate a systematic noise floor for bright stars of ~0.2% rms null leakage uncertainty per observing cluster in the broadband channel. A similar analysis is performed for the narrowband channels. We also provide additional information needed for science reduction, including details on the instrument beam pattern and the basic astrophysical response of the system, and references to the data reduction and modeling tools
A cosmologically motivated description of the dark matter halo profile for the Low Surface Brightness Galaxy, Malin 1
In this paper we derive a possible mass profile for the low surface
brightness galaxy, Malin 1, based upon previously published space-based and
ground-based photometric properties and kinematics. We use properties of the
bulge, normal disk, outer extended disk and \ion{H}{1} mass as inputs into mass
profile models. We find that the dark matter halo model of Malin 1 is best
described by a halo profile that has undergone adiabatic contraction,
inconsistent with the findings for most disk galaxies to date, yet consistent
with rotation curve studies of M31. More importantly, we find that Malin 1 is
baryon dominated in its central regions out to a radius of kpc (in the
bulge region). Low-surface brightness galaxies are often referred to as being
dark matter dominated at all radii. If this is the case, then Malin 1 would
seem to have characteristics similar to those of normal barred disk galaxies,
as suggested by other recent work. We also find that Malin 1 also falls on the
rotation curve shear versus spiral arm pitch angle relation for normal
galaxies, although more LSB galaxies need to be studied to determine if this is
typical.Comment: 10 pages, 3 figures (1 color), accepted for publication in PAS
Boojums and the Shapes of Domains in Monolayer Films
Domains in Langmuir monolayers support a texture that is the two-dimensional
version of the feature known as a boojum. Such a texture has a quantifiable
effect on the shape of the domain with which it is associated. The most
noticeable consequence is a cusp-like feature on the domain boundary. We report
the results of an experimental and theoretical investigation of the shape of a
domain in a Langmuir monolayer. A further aspect of the investigation is the
study of the shape of a ``bubble'' of gas-like phase in such a monolayer. This
structure supports a texture having the form of an inverse boojum. The
distortion of a bubble resulting from this texture is also studied. The
correspondence between theory and experiment, while not perfect, indicates that
a qualitative understanding of the relationship between textures and domain
shapes has been achieved.Comment: replaced with published version, 10 pages, 13 figures include
The Hubble Space Telescope Key Project on the Extragalactic Distance Scale XXIV: The Calibration of Tully-Fisher Relations and the Value of the Hubble Constant
This paper presents the calibration of BVRIH$ Tully-Fisher relations based on
Cepheid distances to 21 galaxies within 25 Mpc, and 23 clusters within 10,000
km/s. These relations have been applied to several distant cluster surveys in
order to derive a value for the Hubble constant, H0, mainly concentrating on an
I-band all-sky survey by Giovanelli and collaborators which consisted of total
I magnitudes and 50% linewidth data for ~550 galaxies in 16 clusters. For
comparison, we also derive the values of H0 using surveys in B-band and V-band
by Bothun and collaborators, and in H-band by Aaronson and collaborators.
Careful comparisons with various other databases from literature suggest that
the H-band data, whose magnitudes are isophotal magnitudes extrapolated from
aperture magnitudes rather than total magnitudes, are subject to systematic
uncertainties. Taking a weighted average of the estimates of Hubble constants
from four surveys, we obtain H0 = 71 +- 4 (random) +- 7 (systematic) km/s/Mpc.
We have also investigated how various systematic uncertainties affect the value
of H0 such as the internal extinction correction method used, Tully-Fisher
slopes and shapes, a possible metallicity dependence of the Cepheid
period-luminosity relation and cluster population incompleteness bias.Comment: 34 pages, 13 figure
The mass function of the Las Campanas loose groups of galaxies
We have determined the mass function of loose groups of galaxies in the Las
Campanas Redshift Survey. Loose groups of galaxies in the LCRS range in mass
from M \sim 10^{12} {\rm M}_{\sun} to 10^{15} {\rm M}_{\sun}. We find that
the sample is almost complete for masses in the interval 5\cdot 10^{13}-8\cdot
10^{14} {\rm M}_{\sun}. Comparison of the observed mass function with
theoretical mass functions obtained from N-body simulations shows good
agreement with a CDM model with the parameters ,
and the amplitude of perturbations about
. For smaller masses the mass function of LCRS loose groups
flattens out, differing considerably from the group mass function found by
Girardi and Giuricin (2000) and from mass functions obtained by numerical
simulations.Comment: 9 pages, 7 figures, AA accepte
The dusty AGB star RS CrB: first mid-infrared interferometric observations with the Keck Telescopes
We report interferometric observations of the semi-regular variable star RS
CrB, a red giant with strong silicate emission features. The data were among
the first long baseline mid-infrared stellar fringes obtained between the Keck
telescopes, using parts of the new nulling beam combiner. The light was
dispersed by a low-resolution spectrometer, allowing simultaneous measurement
of the source visibility and intensity spectra from 8 to 12 microns. The
interferometric observations allow a non-ambiguous determination of the dust
shell spatial scale and relative flux contribution. Using a simple
spherically-symmetric model, in which a geometrically thin shell surrounds the
stellar photosphere, we find that ~30% to ~70% of the overall mid-infrared flux
- depending on the wavelength - originates from 7-8 stellar radii. The derived
shell opacity profile shows a broad peak around 11 microns (tau ~ 0.06),
characteristic of Mg-rich silicate dust particles.Comment: Accepted for publication in ApJ Letter
Thermodynamic glass transition in a spin glass without time-reversal symmetry
Spin glasses are a longstanding model for the sluggish dynamics that appears
at the glass transition. However, spin glasses differ from structural glasses
for a crucial feature: they enjoy a time reversal symmetry. This symmetry can
be broken by applying an external magnetic field, but embarrassingly little is
known about the critical behaviour of a spin glass in a field. In this context,
the space dimension is crucial. Simulations are easier to interpret in a large
number of dimensions, but one must work below the upper critical dimension
(i.e., in d<6) in order for results to have relevance for experiments. Here we
show conclusive evidence for the presence of a phase transition in a
four-dimensional spin glass in a field. Two ingredients were crucial for this
achievement: massive numerical simulations were carried out on the Janus
special-purpose computer, and a new and powerful finite-size scaling method.Comment: 10 pages, 6 figure
- …