169 research outputs found
Synthetic hydrogen spectra of prominence oscillations
Context. Prominence oscillations have been mostly detected using Doppler
velocity, although there are also claimed detections by means of periodic
variations in half-width or line intensity. However, scarce observational
evidence exists about simultaneous detection of oscillations in several
spectral indicators. Aims. Our main aim here is to explore the relationship
between spectral indicators, such as Doppler shift, line intensity, and line
half-width, and the linear perturbations excited in a simple prominence model.
Methods. Our equilibrium background model consists of a bounded, homogeneous
slab, which is permeated by a transverse magnetic field, having prominence-like
physical properties. Assuming linear perturbations, the dispersion relation for
fast and slow modes has been derived, as well as the perturbations for the
different physical quantities. These perturbations have been used as the input
variables in a one-dimensional radiative transfer code, which calculates the
full spectral profile of the hydrogen H-alpha and H-beta lines. Results. We
have found that different oscillatory modes produce spectral indicator
variations in different magnitudes. Detectable variations in the Doppler
velocity were found for the fundamental slow mode only. Substantial variations
in the H-beta line intensity were found for specific modes. Other modes lead to
lower and even undetectable parameter variations. Conclusions. To perform
prominence seismology, analysis of the H-alpha and H-beta spectral line
parameters could be a good tool to detect and identify oscillatory modes.Comment: 9 pages, 6 figures, 2 tables, accepted for publication in Astronomy
and Astrophysic
Dark Off-limb Gap:Manifestation of a Temperature Minimum and the Dynamic Nature of the Chromosphere
We study off-limb emission of the lower solar atmosphere using
high-resolution imaging spectroscopy in the H and Ca II 8542 \r{A} lines
obtained with the CHROMospheric Imaging Spectrometer (CHROMIS) and the CRisp
Imaging SpectroPolarimeter (CRISP) on the Swedish 1-m Solar Telescope. The
H line wing images show the dark intensity gap between the photospheric
limb and chromosphere which is absent in the Ca II images. We calculate
synthetic spectra of the off-limb emissions with the RH code in the
one-dimension spherical geometry and find good agreement with the observations.
The analysis of synthetic line profiles shows that the gap in the H line
wing images maps the temperature minimum region between the photosphere and
chromosphere due to the well known opacity and emissivity gap of Balmer lines
in this layer. However, observed gap is detected farther from the line core in
the outer line wing positions than in the synthetic profiles. We found that an
increased microturbulence in the model chromosphere is needed to reproduce the
dark gap in the outer line wing, suggesting that observed H gap is the
manifestation of the temperature minimum and the dynamic nature of the solar
chromosphere. The temperature minimum produces a small enhancement in synthetic
Ca II line-wing intensities. Observed off-limb Ca II line-wing emissions show
similar enhancement below temperature minimum layer near the edge of the
photospheric limb.Comment: 14 pages, 8 figures, accepted in Ap
Quiescent prominences in the era of ALMA : simulated observations using 3D whole-prominence fine structure model
We use the detailed 3D whole-prominence fine structure model to produce the first simulated high-resolution ALMA observations of a modeled quiescent solar prominence. The synthetic brightness temperature and optical thickness maps shown in the present paper are produced using a visualization method for the sub-millimeter/millimeter radio continua synthesis. We have obtained the simulated observations of both the prominence at the limb and the filament on the disk at wavelengths covering a broad range which encompasses the full potential of ALMA.We demonstrate here to what extent the small-scale and large-scale prominence and filament structures will be visible in the ALMA observations spanning both the optically thin and thick regimes. We analyze the relationship between the brightness and kinetic temperature of the prominence plasma. We also illustrate the opportunities ALMA will provide for studying the thermal structure of the prominence plasma from the cool prominence fine structure cores to the prominence-corona transition region. In addition, we show that the detailed 3D modeling of entire prominences with their numerous fine structures will be important for the correct interpretation of future ALMA prominence observations.PostprintPeer reviewe
Quiescent prominences in the era of ALMA. II. Kinetic temperature diagnostics
Funding: UK STFC, the Leverhulme Trust, and NASA (D.H.M.)We provide the theoretical background for diagnostics of the thermal properties of solar prominences observed by the Atacama Large Millimeter/submillimeter Array (ALMA). To do this, we employ the 3D Whole-Prominence Fine Structure (WPFS) model that produces synthetic ALMA-like observations of a complex simulated prominence. We use synthetic observations derived at two different submillimeter/millimeter (SMM) wavelengths—one at a wavelength at which the simulated prominence is completely optically thin and another at a wavelength at which a significant portion of the simulated prominence is optically thick—as if these were the actual ALMA observations. This allows us to develop a technique for an analysis of the prominence plasma thermal properties from such a pair of simultaneous high-resolution ALMA observations. The 3D WPFS model also provides detailed information about the distribution of the kinetic temperature and the optical thickness along any line of sight. We can thus assess whether the measure of the kinetic temperature derived from observations accurately represents the actual kinetic temperature properties of the observed plasma. We demonstrate here that in a given pixel the optical thickness at the wavelength at which the prominence plasma is optically thick needs to be above unity or even larger to achieve a sufficient accuracy of the derived information about the kinetic temperature of the analyzed plasma. Information about the optical thickness cannot be directly discerned from observations at the SMM wavelengths alone. However, we show that a criterion that can identify those pixels in which the derived kinetic temperature values correspond well to the actual thermal properties in which the observed prominence can be established.Publisher PDFPeer reviewe
Observing the Solar Chromosphere
This review is split into two parts: one on chromospheric line formation in
answer to the frequent question "where is my line formed", and one presenting
state-of-the-art imagery of the chromosphere. In the first part I specifically
treat the formation of the Na D lines, Ca II H & K, and Halpha. In the second I
show DOT, IBIS, VAULT, and TRACE images as evidence that the chromosphere
consists of fibrils of intrinsically different types. The straight-up ones are
hottest. The slanted ones are filled by shocks and likely possess thin
transition sheaths to coronal plasma. The ones hovering horizontally over
"clapotispheric" cell interiors outline magnetic canopies and are buffeted by
shocks, most violently in the quietest regions. In the absence of
integral-field ultraviolet spectrometry, H remains the principal
chromosphere diagnostic. The required fast-cadence profile-sampling imaging is
an important quest for new telescope technology.Comment: in press,"Physics of Chromospheric Plasmas" (Coimbra), ASP 368, 27
(2007
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