382 research outputs found
Estimates of Active Region Area Coverage through Simultaneous Measurements of He I 5876 and 10830 Lines
Simultaneous, high-quality measurements of the neutral helium triplet
features at 5876~\AA\ and 10830~\AA, respectively, in a sample of solar-type
stars are presented. The observations were made with ESO telescopes at the La
Silla Paranal Observatory under program ID 088.D-0028(A) and MPG Utility Run
for FEROS 088.A-9029(A). The equivalent widths of these features combined with
chromospheric models are utilized to infer the fractional area coverage, or
filling factor, of magnetic regions outside of spots. We find that the majority
of the sample is characterized by filling factors less than unity. However,
discrepancies occur among the coolest K-type and warmest and most rapidly
rotating F-type dwarf stars. We discuss these apparently anomalous results and
find that in the case of K-type stars they are an artifact of the application
of chromospheric models best suited to the Sun than to stars with significantly
lower . The case of the F-type rapid rotators can be explained
with the measurement uncertainties of the equivalent widths, but they may also
be due to a non-magnetic heating component in their atmospheres. With the
exceptions noted above, preliminary results suggest that the average heating
rates in the active regions are the same from one star to the other, differing
in the spatially integrated, observed level of activity due to the area
coverage. Hence, differences in activity in this sample are mainly due to the
filling factor of active regions.Comment: Accepted for publication in The Astrophysical Journa
Searching for links between magnetic fields and stellar evolution. I. A survey of magnetic fields in open cluster A- and B-type stars with FORS1
About 5% of upper main sequence stars are permeated by a strong magnetic
field, the origin of which is still matter of debate.
With this work we provide observational material to study how magnetic fields
change with the evolution of stars on the main sequence, and to constrain
theory explaining the presence of magnetic fields in A and B-type stars.
Using FORS1 in spectropolarimetric mode at the ESO VLT, we have carried out a
survey of magnetic fields in early-type stars belonging to open clusters and
associations of various ages.
We have measured the magnetic field of 235 early-type stars with a typical
uncertainty of about 100 G. In our sample, 97 stars are Ap or Bp stars. For
these targets, the median error bar of our field measurements was about 80 G. A
field has been detected in about 41 of these stars, 37 of which were not
previously known as magnetic stars. For the 138 normal A and B-type stars, the
median error bar was 136 G, and no field was detected in any of them.Comment: Accepted by A&A; 15 pages (article)+15 pages (tables), 8 figure
ITALIAN VALIDATION OF PELVIC PAIN AND URGENCY/FREQUENCY PATIENTS SYMPTOMS SCALE (PUF) QUESTIONNAIRE
Coordination within the remote sensing payload on the Solar Orbiter mission
Context. To meet the scientific objectives of the mission, the Solar Orbiter spacecraft carries a suite of in-situ (IS) and remote sensing (RS) instruments designed for joint operations with inter-instrument communication capabilities. Indeed, previous missions have shown that the Sun (imaged by the RS instruments) and the heliosphere (mainly sampled by the IS instruments) should be considered as an integrated system rather than separate entities. Many of the advances expected from Solar Orbiter rely on this synergistic approach between IS and RS measurements. /
Aims. Many aspects of hardware development, integration, testing, and operations are common to two or more RS instruments. In this paper, we describe the coordination effort initiated from the early mission phases by the Remote Sensing Working Group. We review the scientific goals and challenges, and give an overview of the technical solutions devised to successfully operate these instruments together. /
Methods. A major constraint for the RS instruments is the limited telemetry (TM) bandwidth of the Solar Orbiter deep-space mission compared to missions in Earth orbit. Hence, many of the strategies developed to maximise the scientific return from these instruments revolve around the optimisation of TM usage, relying for example on onboard autonomy for data processing, compression, and selection for downlink. The planning process itself has been optimised to alleviate the dynamic nature of the targets, and an inter-instrument communication scheme has been implemented which can be used to autonomously alter the observing modes. We also outline the plans for in-flight cross-calibration, which will be essential to the joint data reduction and analysis. /
Results. The RS instrument package on Solar Orbiter will carry out comprehensive measurements from the solar interior to the inner heliosphere. Thanks to the close coordination between the instrument teams and the European Space Agency, several challenges specific to the RS suite were identified and addressed in a timely manner
Curcumin Modulates Nitrosative Stress, Inflammation, and DNA Damage and Protects against Ochratoxin A-Induced Hepatotoxicity and Nephrotoxicity in Rats.
Ochratoxin A (OTA) is a fungal toxin of critical concern for food safety both for human
health and several animal species, also representing a cancer threat to humans. Curcumin (CURC) is
a natural polyphenol that has anti-apoptotic, anti-inflammatory, and antioxidant effects. The aim
of this study was to investigate the cytoprotective effect of CURC against OTA-induced nephrotoxicity and hepatotoxicity through the study of the nitrosative stress, pro-inflammatory cytokines,
and deoxyribonucleic acid (DNA) damage. Sprague Dawley rats were daily treated with CURC
(100 mg/kg b.w.), OTA (0.5 mg/kg b.w), or CURC with OTA by oral gavage for 14 days. Our results
demonstrated that OTA exposure was associated with significant increase of pro-inflammatory and
DNA oxidative-damage biomarkers. Moreover, OTA induced the inducible nitric oxide synthase,
(iNOS) resulting in increased nitric oxide (NO) levels both in kidney and liver. The co-treatment
OTA + CURC counteracted the harmful effects of chronic OTA treatment by regulating inflammation,
reducing NO levels and oxidative DNA damage in kidney and liver tissues. Histology revealed that
OTA + CURC treatment determinates mainly an Iba1+ macrophagic infiltration with fewer CD3+
T-lymphocytes in the tissues. In conclusion, we evidenced that CURC exerted cytoprotective and
antioxidant activities against OTA-induced toxicity in rats
VV Pup in a low state: secondary-star irradiation or stellar activity?
Aims. Emission lines in polars show complex profiles with multiple components
that are typically ascribed to the accretion stream, threading region,
accretion spot, and the irradiated secondary-star. In low-state polars the
fractional contribution by the accretion stream, and the accretion spot is
greatly reduced offering an opportunity to study the effect of the
secondary-star irradiation or stellar activity. We observed VV Pup during an
exceptional low-state to study and constrain the properties of the line-forming
regions and to search for evidence of chromospheric activity and/or
irradiation. Methods. We obtained phase-resolved optical spectra at the ESO
VLT+FORS1 with the aim of analyzing the emission line profile and radial
velocity as a function of the orbital period. We also tailored irradiated
secondary-star models to compare the predicted and the observed emission lines
and to establish the nature of the line-forming regions. Results. Our
observations and data analysis, when combined with models of the irradiated
secondary-star, show that, while the weak low ionization metal lines (FeI and
MgI) may be consistent with irradiation processes, the dominant Balmer H
emission lines, as well as NaI and HeI, cannot be reproduced by the irradiated
secondary-star models. We favor the secondary-star chromospheric activity as
the main forming region and cause of the observed H, NaI, and He emission
lines, though a threading region very close to the L1 point cannot be excluded.Comment: 10 pages, 9 figures, in press on A&
The Solar Radius in the EUV during the Cycle XXIII
Aims. To determine the solar transition region and coronal radius at EUV
wavelengths and its time evolution during Solar Cycle XXIII.
Methods. We use daily 30.4 and 17.1 nm images obtained by the Extreme
Ultraviolet Imager (EIT) aboard the SoHO satellite and derive the solar radius
by fitting a circle to the limb brightness ring.
Results. The weighted mean of the temporal series gives (967''.56 +/- 0''.04)
and (969''.54 +/- 0''.02) at 30.4 and 17.1 nm respectively. No significant
correlation was found with the solar cycle at any of the two wavelengths.
Conclusions. Since the temperature formation of the 30.4 nm line is between
(60 - 80) 10^3 K (Transition Region), the obtained result is bigger than that
derived from present atmospheric models. On the contrary this height is
compatible with radio models.Comment: accepted for publication in Astronomy & Astrophysics minor changes
introduced during review proces
Potential Approaches Versus Approved or Developing Chronic Myeloid Leukemia Therapy.
Tyrosine kinase inhibitors (TKIs) have revolutionized the treatment of patients with chronic myeloid leukemia (CML). However, continued use of these inhibitors has contributed to the increase in clinical resistance and the persistence of resistant leukemic stem cells (LSCs). So, there is an urgent need to introduce additional targeted and selective therapies to eradicate quiescent LSCs, and to avoid the relapse and disease progression. Here, we focused on emerging BCR-ABL targeted and non-BCR-ABL targeted drugs employed in clinical trials and on alternative CML treatments, including antioxidants, oncolytic virus, engineered exosomes, and natural products obtained from marine organisms that could pave the way for new therapeutic approaches for CML patients
Comparing extrapolations of the coronal magnetic field structure at 2.5 solar radii with multi-viewpoint coronagraphic observations
The magnetic field shapes the structure of the solar corona but we still know
little about the interrelationships between the coronal magnetic field
configurations and the resulting quasi-stationary structures observed in
coronagraphic images (as streamers, plumes, coronal holes). One way to obtain
information on the large-scale structure of the coronal magnetic field is to
extrapolate it from photospheric data and compare the results with
coronagraphic images. Our aim is to verify if this comparison can be a fast
method to check systematically the reliability of the many methods available to
reconstruct the coronal magnetic field. Coronal fields are usually extrapolated
from photospheric measurements typically in a region close to the central
meridian on the solar disk and then compared with coronagraphic images at the
limbs, acquired at least 7 days before or after to account for solar rotation,
implicitly assuming that no significant changes occurred in the corona during
that period. In this work, we combine images from three coronagraphs
(SOHO/LASCO-C2 and the two STEREO/SECCHI-COR1) observing the Sun from different
viewing angles to build Carrington maps covering the entire corona to reduce
the effect of temporal evolution to ~ 5 days. We then compare the position of
the observed streamers in these Carrington maps with that of the neutral lines
obtained from four different magnetic field extrapolations, to evaluate the
performances of the latter in the solar corona. Our results show that the
location of coronal streamers can provide important indications to discriminate
between different magnetic field extrapolations.Comment: Accepted by A&A the 20th of May, 201
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