adsabs/AstroCLIMB huggingface dataset:
Paper: CLASS Observations of Atmospheric Cloud Polarization at millimeter Wavelengths
Authors: Yunyang Li, 云炀 李, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Jullianna Denes Couto, Sumit Dahal, Rahul Datta, Rolando Dünner, Joseph R. Eimer, Thomas Essinger-Hileman, Kathleen Harrington, Jeffrey Iuliano, Tobias A. Marriage, Matthew A. Petroff, Rodrigo A. Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Oliver F. Wolff, Edward J. Wollack, Zhilei Xu, 智磊 徐
Figure caption: Illustration of cloud polarization. Clouds containing water droplets and horizontally aligned ice crystals scatter thermal radiation from the ground and the atmosphere, directing linearly polarized radiation into the telescope. The two orthogonal linear polarization states are labeled; they correspond to the Q (0°, in orange) and −Q (90°, i.e., horizontal, in blue) Stokes parameter evaluated in the horizontal frame of the telescope. Clouds are depicted as cumulus clouds instead of cirrus for their aesthetic appeal. Objects are not to scale.
Paper: CLASS Observations of Atmospheric Cloud Polarization at millimeter Wavelengths
Authors: Yunyang Li, 云炀 李, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Jullianna Denes Couto, Sumit Dahal, Rahul Datta, Rolando Dünner, Joseph R. Eimer, Thomas Essinger-Hileman, Kathleen Harrington, Jeffrey Iuliano, Tobias A. Marriage, Matthew A. Petroff, Rodrigo A. Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Oliver F. Wolff, Edward J. Wollack, Zhilei Xu, 智磊 徐
Figure caption: Polarized signal from Rayleigh scattering of thermal emission from the ground and the atmosphere for different cloud particle shapes. Assuming homogeneous spheroidal cloud particles with uniform dielectric properties, the particle shape is parameterized by its aspect ratio, or equivalently, the depolarization factor Δ z . The linear polarization from an ensemble of randomly oriented cloud particles with the short axis aligned vertically is computed for each of the four CLASS frequency bands (color coded), for different cloud heights above the ground (5200  m above sea level), with a total 2 mm PWV. The cloud height and PWV determine the optical loading above the cloud (Equation (3)), and impact the polarization from the forward scattering of atmospheric emission, especially at higher frequencies. Top: the Stokes Q polarization signal in units of brightness temperature for a reference optical depth τ  ν  equivalent to IWP = 10 g m−2 and particle diameter D = 100 μm (geometric mean of the three axes). Bottom: the corresponding polarization fraction. Signed values are used to distinguish the sign of Stokes Q polarizations.
Paper: CLASS Observations of Atmospheric Cloud Polarization at millimeter Wavelengths
Authors: Yunyang Li, 云炀 李, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Jullianna Denes Couto, Sumit Dahal, Rahul Datta, Rolando Dünner, Joseph R. Eimer, Thomas Essinger-Hileman, Kathleen Harrington, Jeffrey Iuliano, Tobias A. Marriage, Matthew A. Petroff, Rodrigo A. Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Oliver F. Wolff, Edward J. Wollack, Zhilei Xu, 智磊 徐
Figure caption: Aerial view of the CLASS site. The background image shows the CLASS site and its surrounding terrain; the two CLASS telescope mounts are slightly off-center. The direction toward neighboring CMB experiments on Cerro Toco: POLARBEAR, Atacama Cosmology Telescope (ACT), and the Simons Observatory (SO) are also labeled. Site camera locations and pointings are shown as black wedges, and their FoVs are delineated by the black border lines (solid borders for main cameras 1–3 and dashed ones for cameras that are daytime only). The shaded green region shows the footprint of the CLASS telescopes during the normal constant-elevation scan at 45°. Note that the telescope and camera FoVs are plotted in sky coordinates with the zenith at the center of the image, but the projection of the ground image centers at the nadir direction; therefore, the region enclosed by the site camera border lines do not reflect the actual view of the cameras (the inner border lines are the top edge of the camera images)—only the azimuthal information matches the sky coordinates.
Paper: CLASS Observations of Atmospheric Cloud Polarization at millimeter Wavelengths
Authors: Yunyang Li, 云炀 李, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Jullianna Denes Couto, Sumit Dahal, Rahul Datta, Rolando Dünner, Joseph R. Eimer, Thomas Essinger-Hileman, Kathleen Harrington, Jeffrey Iuliano, Tobias A. Marriage, Matthew A. Petroff, Rodrigo A. Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Oliver F. Wolff, Edward J. Wollack, Zhilei Xu, 智磊 徐
Figure caption: Cloud fraction and water content profile near the CLASS site from 2016 August to 2022 May derived from ERA5 (Hersbach et al. 2020) per pressure level hourly data. The pressure levels are converted into altitudes above sea level (top axis) using the annually averaged atmosphere profile from Molod et al. (2015) and the hydrostatic equation. Top: cloud cover fraction as a function of atmospheric pressure (altitude). This quantity is the proportion of a grid box covered by cloud in the ERA5 model. Bottom: the specific cloud water content in the liquid (darker blue) and ice (lighter blue) phases. The area enclosed under the curves (in linear pressure axis) is proportional to the liquid- (Ice-) water path. In both panels, the solid curves show the mean value at given pressure levels; the shaded regions fill between the 50th and 95th percentiles of the distribution. Due to aridness at the queried region, the 50th percentiles are essentially zero. The vertical dotted line marks the altitude where the median air temperature is −40°C, above which (altitude) homogeneous nucleation occurs.
Paper: CLASS Observations of Atmospheric Cloud Polarization at millimeter Wavelengths
Authors: Yunyang Li, 云炀 李, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Jullianna Denes Couto, Sumit Dahal, Rahul Datta, Rolando Dünner, Joseph R. Eimer, Thomas Essinger-Hileman, Kathleen Harrington, Jeffrey Iuliano, Tobias A. Marriage, Matthew A. Petroff, Rodrigo A. Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Oliver F. Wolff, Edward J. Wollack, Zhilei Xu, 智磊 徐
Figure caption: Cloud polarization spectrum ratio between the Mie solution and the Rayleigh scattering approximation for spherical ice particles. The colored lines show the ratio evaluated for a homogeneous population with particle diameters ranging from 300 –400 μm. The black curve shows the average result from a population of ice particles with log-normal size distribution at −70 °C (Austin et al. 2009). CLASS observation frequencies and bandwidths are shown as the shaded vertical bands.
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: The measured VSWR profiles of the 50–500 MHz prototype LPDA. Solid-gray line: response with design specification as given in Table 1. Dotted-gray line: response with design specification (except the last column) as given in Table 2. Dashed-gray line: response after implementing the suggestion given in Section 2.4.1. Solid-black line: response after implementing the suggestions in Sections 2.4.1 and 2.4.2.
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: Schematic showing top view of the CLPDA with rectangular bar transmission lines; the X1 and X2/Y1 and Y2 pair holds the dipole elements oriented horizontally/vertically.
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: Schematic of the CLPDA with boom transmission lines; the H1 and H2/V1 and V2 pair holds the dipole elements oriented horizontally (X-pol.)/vertically (Y-pol.).
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: Same as Figure 9, but shown from the side view.
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: Plot of LPDA directional gain as a function of design parameters τ and σ (reproduced from Carrel 1961a).
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: Smith chart of the prototype LPDA after introducing dipoles of different diameters and adjusting the inter-boom spacing; the corresponding parameter values are listed in Table 2.
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: The ratio of electrical length (L e) to physical length (L p) of a dipole is plotted against the ratio of its physical length to diameter (d). Measurements taken with aluminum cylindrical tubes of outer diameter 13, 8, and 6 mm are shown with the “circle,” “square,” and “diamond” symbols, respectively. A vertical dotted line is drawn at L p/d = 80, in order to show that L e/L p approaches unity asymptotically beyond that.
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: VSWR of the prototype LPDA as a function of frequency; the horizontal line drawn at VSWR equal to 2.0 shows a power transmission of ≈90%. The design specifications of the LPDA are given in Table 1.
Paper: Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna
Authors: Anshu Kumari, G. V. S. Gireesh, C. Kathiravan, V. Mugundhan, Indrajit V. Barve, R. Ramesh, C. Monstein
Figure caption: Simulated VSWR using 4NEC2. The dashed and solid lines correspond to the LPDA with 17 and 22 dipoles, respectively.
Paper: Generation of Subion Scale Magnetic Holes from Electron Shear Flow Instabilities in Plasma Turbulence
Authors: Giuseppe Arrò, Francesco Pucci, Francesco Califano, Maria Elena Innocenti, Giovanni Lapenta
Figure caption: Time sequence describing the formation of a subion scale magnetic hole from large scale turbulent fluctuations. Shaded isocontours represent the out-of-plane magnetic field fluctuations δ B  z  (in units of B 0) while black streamlines indicate the in-plane electron fluid velocity in the frame comoving with the local center of mass velocity ﹩{\boldsymbol{u}}{{\prime} }_{e}﹩.
Paper: Generation of Subion Scale Magnetic Holes from Electron Shear Flow Instabilities in Plasma Turbulence
Authors: Giuseppe Arrò, Francesco Pucci, Francesco Califano, Maria Elena Innocenti, Giovanni Lapenta
Figure caption: First example of EVMH at ﹩t=650\,{{\rm{\Omega }}}_{e}^{-1}﹩. (a) Shaded isocontours represent the magnetic field magnitude (in units of B 0) while black lines indicate the in-plane magnetic field lines. (b) Shaded isocontours represent the electron temperature anisotropy T  e,⊥/T  e,∥ − 1, black streamlines indicate the in-plane electron fluid velocity ﹩{\boldsymbol{u}}{{\prime} }_{e}﹩ while the yellow square box highlights the region where the EVDF is calculated. (c) 3D isosurfaces of the EVDF, with the red arrow indicating the direction of the local magnetic field. (d)–(f) 2D projections of the EVDF in the directions parallel and perpendicular to the local magnetic field.
Paper: Generation of Subion Scale Magnetic Holes from Electron Shear Flow Instabilities in Plasma Turbulence
Authors: Giuseppe Arrò, Francesco Pucci, Francesco Califano, Maria Elena Innocenti, Giovanni Lapenta
Figure caption: Third example of a couple of EVMHs at ﹩t=650\,{{\rm{\Omega }}}_{e}^{-1}﹩. (a) Shaded isocontours represent the magnetic field magnitude (in units of B 0) while black lines indicate the in-plane magnetic field lines. (b) Shaded isocontours represent the electron temperature anisotropy T  e,⊥/T  e,∥ − 1, black streamlines indicate the in-plane electron fluid velocity ﹩{\boldsymbol{u}}{{\prime} }_{e}﹩ while the yellow and green square boxes highlight the regions where the EVDFs are calculated.
Paper: Generation of Subion Scale Magnetic Holes from Electron Shear Flow Instabilities in Plasma Turbulence
Authors: Giuseppe Arrò, Francesco Pucci, Francesco Califano, Maria Elena Innocenti, Giovanni Lapenta
Figure caption: 3D isosurfaces of the EVDFs calculated on the edge (a) and in the center (b) of the EVMH of Figure 6, with red arrows indicating the direction of the local magnetic field. 2D projections of the EVDF in the directions parallel and perpendicular to the local magnetic field, referred to the edge (c)–(e) and to the center (f)–(h) of the EVMH.
Paper: Generation of Subion Scale Magnetic Holes from Electron Shear Flow Instabilities in Plasma Turbulence
Authors: Giuseppe Arrò, Francesco Pucci, Francesco Califano, Maria Elena Innocenti, Giovanni Lapenta
Figure caption: Left panels: close-up of the electron velocity shear at ﹩t=325\,{{\rm{\Omega }}}_{e}^{-1}﹩ (a), and ﹩t=425\,{{\rm{\Omega }}}_{e}^{-1}﹩ (c), where shaded isocontours indicate δ B  z  (in units of B 0), black streamlines represent the in-plane electron fluid velocity ﹩{\boldsymbol{u}}{{\prime} }_{e}﹩, and the yellow solid arrow indicates the direction of the transversal cut through the velocity shear. Right panels: electron fluid velocity longitudinal to the shear flow ﹩{u}_{e,L}^{\prime} ﹩, threshold velocity V KH and electron velocity jump Δu  e  (between the two purple dots) over the transversal cut at ﹩t=325\,{{\rm{\Omega }}}_{e}^{-1}﹩ (b), and ﹩t=425\,{{\rm{\Omega }}}_{e}^{-1}﹩ (d) (all velocities are in units of the initial Alfvén speed c  A , and the horizontal dotted line is located at zero).
Paper: Generation of Subion Scale Magnetic Holes from Electron Shear Flow Instabilities in Plasma Turbulence
Authors: Giuseppe Arrò, Francesco Pucci, Francesco Califano, Maria Elena Innocenti, Giovanni Lapenta
Figure caption: Panels (a)–(c): shaded isocontours of the magnetic field magnitude (in units of B 0) over the whole simulation box at ﹩t=650\,{{\rm{\Omega }}}_{e}^{-1}﹩, with a progressive zoom into an EVMH. Panels (d)–(i): magnetic field (in units of B 0), electron and ion number densities (in units of the initial density), electron and ion fluid velocities (in units of the initial Alfvén speed c  A ), electron and ion temperatures (in units of the initial electron temperature) over a 1D cut crossing the EVMH, indicated by the red dashed line in panel (b); black horizontal dashed lines are located at zero, the gray shaded area highlights a region of width 2 d  i  around the EVMH, whose center is indicated by the black vertical dotted line.
Paper: Generation of Subion Scale Magnetic Holes from Electron Shear Flow Instabilities in Plasma Turbulence
Authors: Giuseppe Arrò, Francesco Pucci, Francesco Califano, Maria Elena Innocenti, Giovanni Lapenta
Figure caption: Second example of EVMH at ﹩t=750\,{{\rm{\Omega }}}_{e}^{-1}﹩. All the panels and elements in the figure are organized as in Figure 4.
Paper: The Maximum Energy of Shock-accelerated Cosmic Rays
Authors: Rebecca Diesing
Figure caption: PeV to GeV proton luminosity ratio (L PeV/L GeV) as a function of v sh for SNR PeVatron candidates, i.e., data points from Figure 3 with ﹩{E}_{\max }\gt {10}^{6}﹩ GeV. Shock age is denoted with the color scale. Due to the postcursor effect (Diesing & Caprioli 2021, see text for details), faster shocks—which are the best candidates to accelerate PeV particles—likely produce steeper spectra, and thus exhibit lower L PeV/L GeV. This effect is important for PeVatron searches that select observational targets based on their γ-ray luminosities at lower energies.
Paper: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Jaime de la Cruz Rodríguez, Jorrit Leenaarts
Figure caption: Time and slit plots of magnetic field and Ca II K intensity. Top panel: the photospheric (left) and chromospheric (middle) B LOS, and Ca II K wavelength summed intensity (right). Bottom three panels: temporal evolution of photospheric and chromospheric B LOS, and Ca II K wavelength summed intensity across four slits highlighted in the top panel. In each panel the black contours refer to the enhanced intensity in the Ca II K line.
Paper: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Jaime de la Cruz Rodríguez, Jorrit Leenaarts
Figure caption: Temporal evolution (since 2016-09-16T09:31:29 UT) and stratification of physical parameters obtained from non-LTE inversion. For slit L1, highlighted in Figure 3, the stratification of temperature, LOS velocity, microturbulent velocity, and LOS magnetic field is demonstrated at selected optical depths. The observed and best-fitted Stokes profiles at the locations indicated by colored cross symbols are shown in the Appendix (Figure 12).
Paper: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Jaime de la Cruz Rodríguez, Jorrit Leenaarts
Figure caption: Temporal evolution of a bipolar region across slit L2 shown in Figure 3. The top two panels show B LOS in the photosphere and the chromosphere. The middle panel shows the wavelength summed intensity of the Ca II K line. The bottom two panels show the horizontal magnetic field (B  h ) in the photosphere and total linear polarization (TLP) in the chromosphere. The green and cyan contours indicate the locations of strong (700 G) B  h  (Fe I 6173 Å) and Ca II K intensity, respectively.
Paper: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Jaime de la Cruz Rodríguez, Jorrit Leenaarts
Figure caption: Overview of SST and SDO observations taken on 2016 September 19. (a) Continuum intensity at Fe I 6302 Å superimposed on the HMI continuum intensity. (b) Line-of-sight magnetic field inferred from the Milne–Eddington inversion of the Fe I 6301 line pair superimposed on the HMI magnetogram. (c), (d) Chromospheric intensity maps, observed with the CRISP and CHROMIS instruments at the SST. (e)–(i) AIA images observed in different channels. The blue and red contours indicate negative and positive polarity at the level of 800 G in the photosphere. Solar north is up.
Paper: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Jaime de la Cruz Rodríguez, Jorrit Leenaarts
Figure caption: The magnetic field topology over the EFR. Left panel: the simulated field lines connecting two main patches of opposite polarity. Small-scale loops connecting bipolar regions are highlighted by a yellow box. Right panel: side view of magnetic field topology over the bipolar regions highlighted by the yellow box in the left panel. For better visualization different field lines are displayed in distinct colors. The background image refers to the vertical component of magnetic field (B  z ). The appearance of maximum current density (J) is also highlighted near the PIL.
Paper: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Jaime de la Cruz Rodríguez, Jorrit Leenaarts
Figure caption: Same as Figure 4, but for a region across slit L1 shown in Figure 3.
Paper: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Jaime de la Cruz Rodríguez, Jorrit Leenaarts
Figure caption: DEM integrated over five different temperature bins ranging from log10(T/K) = 5.7 to 7.57. The first four panels show the continuum intensity, B LOS in the photosphere, and Ca II 8542 Å and Ca II K intensity maps. The blue and black contours indicate negative and positive polarities at the 800 G level in the photosphere.
Paper: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Jaime de la Cruz Rodríguez, Jorrit Leenaarts
Figure caption: Overview of emerging flux region (EFR). Left and middle panels: HMI continuum image (left) and LOS magnetogram (middle) saturated at ±1000 G, where black and white colors indicate negative and positive polarities, respectively. The orange box outlines the FOV of SST. Right panel: the temporal evolution of positive and negative magnetic fluxes in the EFR is indicated by solid and dashed black lines, respectively. The vertical gray line marks the time of the SST observation.
Paper: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Jaime de la Cruz Rodríguez, Jorrit Leenaarts
Figure caption: Temporal evolution of DEM (a) and Ca II K summed intensity (b) across the black vertical line shown in Figure 6.
Paper: Extreme Red-wing Enhancements of UV Lines during the 2022 March 30 X1.3 Solar Flare
Authors: Yan Xu, Graham S. Kerr, Vanessa Polito, Nengyi Huang, Ju Jing, Haimin Wang
Figure caption: Temporal evolution of the Si IV (top left), C II (top right; note that all three C II resonance lines are included within this window, two of which are blended), Mg II 2791 Å subordinate line (bottom left), and Mg II k (bottom right). In each, the image represents wavelength vs. time, where the zero-point is indicated in the figure titles. Cutouts at various times are shown also (indicated by the horizontal lines; the thicker horizontal lines are the times for which example Gaussian fits are shown in later figures). In the cutouts, the red vertical lines are the rest wavelengths of the strong lines in each passband. The reference time (t 0) was selected to be the first instance when the red wing of the Mg II resonance lines became broadened during the second brightening of the source of interest.
Paper: Extreme Red-wing Enhancements of UV Lines during the 2022 March 30 X1.3 Solar Flare
Authors: Yan Xu, Graham S. Kerr, Vanessa Polito, Nengyi Huang, Ju Jing, Haimin Wang
Figure caption: Spectra from the SOI, where the extremely broadened, redshifted wings are obvious. Shown are C II (top left), O I 1355.6 Å (top-middle), Si IV (top right), Mg II (bottom row, including a zoomed in view of Mg II k). In each panel, the vertical lines are the rest wavelengths of the main lines within each window. The dotted horizontal line indicates the location of the source of interest. Note that the O I 1355.6 Å does not exhibit a strong Doppler response within the SOI, but is very bright and broadened underneath the main ribbon, which is now in the southmost portion of the field of view. This line does increase a little in intensity after the SOI, perhaps in response to it.