adsabs/AstroCLIMB huggingface dataset:
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption:  T → P leakage probed using survey Moon scan data. Upper limits of 95% confidence interval on T → P leakage estimated from per-detector survey Moon maps plotted with the detector angular distance from the FOV center along the x-axis, and grouped by module. These are estimates for 49 pairs of detectors that are not saturated by the Moon’s signal and include contribution from the Moon’s intrinsic polarization. For module 4, data from only two detector pairs were usable for this analysis. The “×,” “+,” and  represent measurements from −45°, +45°, and pair-differenced detectors, respectively.
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Reimaging optics. The reimaging optics use two lenses to form the image on the focal plane. The location of each element, referenced to the aperture stop, is specified in Table A2. Additional metal-mesh and foam infrared filters are used in the receiver, but these do not impact the optical model.
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Fore-optics design concept. Each mirror is a section of an off-axis ellipsoid with foci indicated by orange circles (for primary), blue circles (for secondary), and mirror center locations indicated by “×” marks, and specified in Table A1. The final image of the stop is indicated by the orange square. This fore-optics system places the entrance pupil on the VPM.
Paper: Light-curve Recovery with Rubin-LSST. II. Unveiling the Darkness of the Galactic Bulge (VESTALE) with RR Lyrae
Authors: M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall'Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, L. Girardi, A. Mazzi, G. Pastorelli, M. Trabucchi, N. Matsunaga, M. Monelli, A. Saha, K. A. Vivas, R. Zanmar Sanchez
Figure caption: Simulated LSST observations during the first 4 yr in ugriz colors (colored points) for two RRL in Saha's sample. Star 3087315 is the faintest in their sample. The orange LC is Saha’s template. Photometric errors (<0.001 mag) derived from OpSim and used in this simulation are too small to be shown.
Paper: Light-curve Recovery with Rubin-LSST. II. Unveiling the Darkness of the Galactic Bulge (VESTALE) with RR Lyrae
Authors: M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall'Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, L. Girardi, A. Mazzi, G. Pastorelli, M. Trabucchi, N. Matsunaga, M. Monelli, A. Saha, K. A. Vivas, R. Zanmar Sanchez
Figure caption: Relative difference (in percentage) between recovered and template periods (top), mean magnitude (middle), and amplitude (bottom) as a function of r mean brightness for the 439 RRL from Saha’s sample. In the middle and top panels the vertical bar reports the accuracy of the recovery of the period.
Paper: Light-curve Recovery with Rubin-LSST. II. Unveiling the Darkness of the Galactic Bulge (VESTALE) with RR Lyrae
Authors: M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall'Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, L. Girardi, A. Mazzi, G. Pastorelli, M. Trabucchi, N. Matsunaga, M. Monelli, A. Saha, K. A. Vivas, R. Zanmar Sanchez
Figure caption: Distance of the template’s average magnitude from the limiting magnitude derived from OpSim for different template distances expressed as factors between new distance and original distance derived from Saha color coded by the σ crowd value. The points below the horizontal line are unlikely to be observed by LSST according to the most recent simulations.
Paper: Light-curve Recovery with Rubin-LSST. II. Unveiling the Darkness of the Galactic Bulge (VESTALE) with RR Lyrae
Authors: M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall'Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, L. Girardi, A. Mazzi, G. Pastorelli, M. Trabucchi, N. Matsunaga, M. Monelli, A. Saha, K. A. Vivas, R. Zanmar Sanchez
Figure caption: Histogram of photometric errors σ crowd due to stellar crowding derived using CrowdingMagUncertMetric.py for the RRL of the Saha sample in the labeled band.
Paper: Light-curve Recovery with Rubin-LSST. II. Unveiling the Darkness of the Galactic Bulge (VESTALE) with RR Lyrae
Authors: M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall'Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, L. Girardi, A. Mazzi, G. Pastorelli, M. Trabucchi, N. Matsunaga, M. Monelli, A. Saha, K. A. Vivas, R. Zanmar Sanchez
Figure caption: Comparison in ugriz bands between Saha’s LC corresponding to the RRL star ID392 and the one obtained by adding the flux of five nearby stars according to TRILEGAL (see text). The difference between the average magnitudes and the amplitudes is reported in each panel.
Paper: Light-curve Recovery with Rubin-LSST. II. Unveiling the Darkness of the Galactic Bulge (VESTALE) with RR Lyrae
Authors: M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall'Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, L. Girardi, A. Mazzi, G. Pastorelli, M. Trabucchi, N. Matsunaga, M. Monelli, A. Saha, K. A. Vivas, R. Zanmar Sanchez
Figure caption: Precision distribution in the recovery of period and average magnitude of RRL in the Saha sample after 1, 2, 3, and 4 yr. The analysis of the right panel shows that, starting from the second year, the precision in the r band remains below 0.04 mag.
Paper: Experimental Scattering Matrices of Martian Dust Aerosols with Narrow Particle-size Distributions
Authors: Julia Martikainen, Olga Muñoz, Juan Carlos Gómez Martín, Teresa Jardiel, Marco Peiteado, Amador C. Caballero, Santiago Pérez-Hoyos, Agustin Sánchez Lavega, Tim Becker, Gerhard Wurm, Yannick Willame, Ann Carine Vandaele
Figure caption: Scattering-angle dependence of the normalized scattering-matrix elements  F  11/ F  11 (30°), − F  12/ F  11,  F  22/ F  11,  F  33/ F  11,  F  34/ F  11, and F  44/ F  11 at 488 nm of the JSC Mars-1, MGS-1, and MMS-2 Martian dust analogs.
Paper: Experimental Scattering Matrices of Martian Dust Aerosols with Narrow Particle-size Distributions
Authors: Julia Martikainen, Olga Muñoz, Juan Carlos Gómez Martín, Teresa Jardiel, Marco Peiteado, Amador C. Caballero, Santiago Pérez-Hoyos, Agustin Sánchez Lavega, Tim Becker, Gerhard Wurm, Yannick Willame, Ann Carine Vandaele
Figure caption: Scattering-angle dependence of the normalized scattering-matrix elements  F  11/ F  11 (30°), − F  12/ F  11,  F  22/ F  11,  F  33/ F  11,  F  34/ F  11, and  F  44/ F  11 at 640 nm of the JSC Mars-1, MGS-1, and MMS-2 Martian dust analogs.
Paper: Experimental Scattering Matrices of Martian Dust Aerosols with Narrow Particle-size Distributions
Authors: Julia Martikainen, Olga Muñoz, Juan Carlos Gómez Martín, Teresa Jardiel, Marco Peiteado, Amador C. Caballero, Santiago Pérez-Hoyos, Agustin Sánchez Lavega, Tim Becker, Gerhard Wurm, Yannick Willame, Ann Carine Vandaele
Figure caption: The observed sky-brightness curves during different atmospheric dust conditions (left panel) at 650 nm. τ = 0.5 corresponds to the normal state of the atmosphere, and τ = 0.8 was obtained during a higher optical depth. The right panels show the measured phase functions of the JSC Mars-1, MMS-2, and MGS-1 analogs for L, M, and S size fractions at 640 nm.
Paper: Experimental Scattering Matrices of Martian Dust Aerosols with Narrow Particle-size Distributions
Authors: Julia Martikainen, Olga Muñoz, Juan Carlos Gómez Martín, Teresa Jardiel, Marco Peiteado, Amador C. Caballero, Santiago Pérez-Hoyos, Agustin Sánchez Lavega, Tim Becker, Gerhard Wurm, Yannick Willame, Ann Carine Vandaele
Figure caption: The linear depolarization ratios for the JSC Mars-1, MGS-1, and MMS-2 L and M samples at 488 and 640 nm.
Paper: Experimental Scattering Matrices of Martian Dust Aerosols with Narrow Particle-size Distributions
Authors: Julia Martikainen, Olga Muñoz, Juan Carlos Gómez Martín, Teresa Jardiel, Marco Peiteado, Amador C. Caballero, Santiago Pérez-Hoyos, Agustin Sánchez Lavega, Tim Becker, Gerhard Wurm, Yannick Willame, Ann Carine Vandaele
Figure caption: The measured scattering-matrix elements of the JSC Mars-1, MGS-1, and MMS-2 L samples at 640 nm.
Paper: Experimental Scattering Matrices of Martian Dust Aerosols with Narrow Particle-size Distributions
Authors: Julia Martikainen, Olga Muñoz, Juan Carlos Gómez Martín, Teresa Jardiel, Marco Peiteado, Amador C. Caballero, Santiago Pérez-Hoyos, Agustin Sánchez Lavega, Tim Becker, Gerhard Wurm, Yannick Willame, Ann Carine Vandaele
Figure caption: The measured scattering-matrix elements of the JSC Mars-1, MGS-1, and MMS-2 L samples at 488 nm.
Paper: Experimental Scattering Matrices of Martian Dust Aerosols with Narrow Particle-size Distributions
Authors: Julia Martikainen, Olga Muñoz, Juan Carlos Gómez Martín, Teresa Jardiel, Marco Peiteado, Amador C. Caballero, Santiago Pérez-Hoyos, Agustin Sánchez Lavega, Tim Becker, Gerhard Wurm, Yannick Willame, Ann Carine Vandaele
Figure caption: SEM images of the S and M samples of the three Martian dust simulants JSC Mars-1, MGS-1, and MMS-2 at higher magnification. These images demonstrate the presence of S particles in the M fractions of MGS-1 and MMS-2. The number at the lower-right corner of the left panels indicates the total length of the scale ruler (horizontal white lines).
Paper: Experimental Scattering Matrices of Martian Dust Aerosols with Narrow Particle-size Distributions
Authors: Julia Martikainen, Olga Muñoz, Juan Carlos Gómez Martín, Teresa Jardiel, Marco Peiteado, Amador C. Caballero, Santiago Pérez-Hoyos, Agustin Sánchez Lavega, Tim Becker, Gerhard Wurm, Yannick Willame, Ann Carine Vandaele
Figure caption: The measured phase functions and P curves of the JSC Mars-1, MGS-1, and MMS-2 M sizes at 488 and 640 nm.
Paper: Experimental Scattering Matrices of Martian Dust Aerosols with Narrow Particle-size Distributions
Authors: Julia Martikainen, Olga Muñoz, Juan Carlos Gómez Martín, Teresa Jardiel, Marco Peiteado, Amador C. Caballero, Santiago Pérez-Hoyos, Agustin Sánchez Lavega, Tim Becker, Gerhard Wurm, Yannick Willame, Ann Carine Vandaele
Figure caption: The measured phase functions and P curves of the JSC Mars-1, MGS-1, and MMS-2 S sizes at 488 and 640 nm.
Paper: Experimental Scattering Matrices of Martian Dust Aerosols with Narrow Particle-size Distributions
Authors: Julia Martikainen, Olga Muñoz, Juan Carlos Gómez Martín, Teresa Jardiel, Marco Peiteado, Amador C. Caballero, Santiago Pérez-Hoyos, Agustin Sánchez Lavega, Tim Becker, Gerhard Wurm, Yannick Willame, Ann Carine Vandaele
Figure caption: The measured scattering-matrix elements of the JSC Mars-1 L analog at 488 and 640 nm.
Paper: Experimental Scattering Matrices of Martian Dust Aerosols with Narrow Particle-size Distributions
Authors: Julia Martikainen, Olga Muñoz, Juan Carlos Gómez Martín, Teresa Jardiel, Marco Peiteado, Amador C. Caballero, Santiago Pérez-Hoyos, Agustin Sánchez Lavega, Tim Becker, Gerhard Wurm, Yannick Willame, Ann Carine Vandaele
Figure caption: The measured scattering-matrix elements of the MMS-2 L analog at 488 and 640 nm.
Paper: Experimental Scattering Matrices of Martian Dust Aerosols with Narrow Particle-size Distributions
Authors: Julia Martikainen, Olga Muñoz, Juan Carlos Gómez Martín, Teresa Jardiel, Marco Peiteado, Amador C. Caballero, Santiago Pérez-Hoyos, Agustin Sánchez Lavega, Tim Becker, Gerhard Wurm, Yannick Willame, Ann Carine Vandaele
Figure caption: The measured scattering-matrix elements of the MGS-1 L analog at 488 and 640 nm.
Paper: Experimental Scattering Matrices of Martian Dust Aerosols with Narrow Particle-size Distributions
Authors: Julia Martikainen, Olga Muñoz, Juan Carlos Gómez Martín, Teresa Jardiel, Marco Peiteado, Amador C. Caballero, Santiago Pérez-Hoyos, Agustin Sánchez Lavega, Tim Becker, Gerhard Wurm, Yannick Willame, Ann Carine Vandaele
Figure caption: Number distributions (left) and projected surface area distributions (right) of the JSC Mars-1, MGS-1, and MMS-2 S, M, and L size fractions.
Paper: Experimental Scattering Matrices of Martian Dust Aerosols with Narrow Particle-size Distributions
Authors: Julia Martikainen, Olga Muñoz, Juan Carlos Gómez Martín, Teresa Jardiel, Marco Peiteado, Amador C. Caballero, Santiago Pérez-Hoyos, Agustin Sánchez Lavega, Tim Becker, Gerhard Wurm, Yannick Willame, Ann Carine Vandaele
Figure caption: The L size fractions of the JSC Mars-1 (left), MGS-1 (middle), and MMS-2 (right) analogs.
Paper: Experimental Scattering Matrices of Martian Dust Aerosols with Narrow Particle-size Distributions
Authors: Julia Martikainen, Olga Muñoz, Juan Carlos Gómez Martín, Teresa Jardiel, Marco Peiteado, Amador C. Caballero, Santiago Pérez-Hoyos, Agustin Sánchez Lavega, Tim Becker, Gerhard Wurm, Yannick Willame, Ann Carine Vandaele
Figure caption: SEM images of the S, M, and L samples of the three Martian dust simulants JSC Mars-1, MGS-1, and MMS-2. The number at the lower-right corner of the left panels indicates the total length of the scale ruler (horizontal white lines).
Paper: Modeling the Magnetic Vectors of Interplanetary Coronal Mass Ejections at Different Heliocentric Distances with INFROS
Authors: Ranadeep Sarkar, Nandita Srivastava, Nat Gopalswamy, Emilia Kilpua
Figure caption: The top panels show the B-field data (in SCEQ coordinates) of the ICME sequentially detected by MESSENGER and VEX for Event 3. The bottom panels depict the same for the ICME sequentially detected by MESSENGER and STEREO-B for Event 4. The black solid lines within the boundary marked by the vertical red lines, denote the magnetic vectors of the ICME. The gray-shaded regions are the ensemble results obtained from the model predictions. The cyan dashed lines represent the ensemble model results corresponding to the lowest impact distance at the outer spacecraft. Among these ensemble model results, the one that best fits the magnetic vectors observed by MESSENGER is denoted as a red dashed line in each plot.
Paper: Modeling the Magnetic Vectors of Interplanetary Coronal Mass Ejections at Different Heliocentric Distances with INFROS
Authors: Ranadeep Sarkar, Nandita Srivastava, Nat Gopalswamy, Emilia Kilpua
Figure caption: Observations of the source region for Event 4. (a) Depicts the morphology of the PEA as observed in the STEREO-B EUVI 195 Å image. The red dashed lines mark the boundary of the PEA region. The green dotted circles denote the location of twin core-dimming regions. (b) Illustrates the line-of-sight component of the HMI magnetic field within the same field-of-view as (b). (a) and (b) are approximately cospatial as the patch center of both images belongs to the same Carrington longitude and latitude. The red dashed boundary and the green dotted circles as shown in (a) are overplotted in panel (b) using the information on their respective Carrington longitude and latitude. The underlying magnetic polarities of the core-dimming locations as denoted by the green dotted circles are shown which indicate a westward-directed left-handed FR.
Paper: Modeling the Magnetic Vectors of Interplanetary Coronal Mass Ejections at Different Heliocentric Distances with INFROS
Authors: Ranadeep Sarkar, Nandita Srivastava, Nat Gopalswamy, Emilia Kilpua
Figure caption: Observations for the source region of Event 6. (a) Depicts the morphology of the PEA as observed in the AIA 211 Å image. The red dashed lines mark the boundary of the PEA region. The green dotted circles denote the location of twin core-dimming regions. (b) Illustrates the line-of-sight component of the HMI magnetic field. The same red dashed boundary and the green dotted circles as shown in (a) are overplotted in panel (b). The underlying magnetic polarities of the core-dimming locations as denoted by the green dotted circles are shown which indicate a southwest-directed left-handed FR.
Paper: Modeling the Magnetic Vectors of Interplanetary Coronal Mass Ejections at Different Heliocentric Distances with INFROS
Authors: Ranadeep Sarkar, Nandita Srivastava, Nat Gopalswamy, Emilia Kilpua
Figure caption: Location of MESSENGER, VEX, STEREO, and Earth in the ecliptic plane during the ICME events under study. The gray-shaded regions denote the propagation path of the ICMEs. The outer boundary of each plot is set at the location of STEREO-B. The Parker spirals are drawn assuming a solar wind speed of 450 km s−1.
Paper: Modeling the Magnetic Vectors of Interplanetary Coronal Mass Ejections at Different Heliocentric Distances with INFROS
Authors: Ranadeep Sarkar, Nandita Srivastava, Nat Gopalswamy, Emilia Kilpua
Figure caption: The top panels depict the CME morphology observed in COR2-B (top-left), LASCO C3 (top-middle), and COR2-A (top-right), respectively for Event 4. The bottom panels illustrate the overplot of the best-fitted wireframe (green dotted marks) of the FR using the GCS model.
Paper: Modeling the Magnetic Vectors of Interplanetary Coronal Mass Ejections at Different Heliocentric Distances with INFROS
Authors: Ranadeep Sarkar, Nandita Srivastava, Nat Gopalswamy, Emilia Kilpua
Figure caption: The top and middle panels show the in situ observations of the total magnetic field and the speed of the solar wind, respectively as obtained by STEREO-B during the ICME Event 1. The two red dashed lines mark the boundary of the MC. The bottom panel is the same as the middle panel but plotted for a 3 month window. The two red solid lines in the bottom panel mark the temporal window within which the top and middle panels are plotted. The cyan dashed lines mark the approximate boundary of the HSS within which the ICME was embedded. The cyan arrows mark the appearance of the same corotating HSS in the previous solar rotations.
Paper: Modeling the Magnetic Vectors of Interplanetary Coronal Mass Ejections at Different Heliocentric Distances with INFROS
Authors: Ranadeep Sarkar, Nandita Srivastava, Nat Gopalswamy, Emilia Kilpua
Figure caption: The black solid lines within the boundary marked by the vertical red lines denote the magnetic vectors (in SCEQ coordinates) of the ICME, which is sequentially observed by MESSENGER and STEREO-B for Event 2. The gray-shaded regions are the model results obtained for Run1. The cyan and magenta colored dashed lines in the right panels denote the model results for Run2 and Run3, respectively.
Paper: Modeling the Magnetic Vectors of Interplanetary Coronal Mass Ejections at Different Heliocentric Distances with INFROS
Authors: Ranadeep Sarkar, Nandita Srivastava, Nat Gopalswamy, Emilia Kilpua
Figure caption: Propagation of the CME leading edge and the associated HSS at different times of the CME evolution from the Sun to 1 au as viewed on the ecliptic plane (Event 1). The black dotted lines denote Parker’s spiral. The gray-shaded region shows the HSS associated with the CME. The curved blue lines depict the CME leading edge. The straight blue lines mark the axis of the two legs of the CME assuming the GCS geometry.
Paper: Modeling the Magnetic Vectors of Interplanetary Coronal Mass Ejections at Different Heliocentric Distances with INFROS
Authors: Ranadeep Sarkar, Nandita Srivastava, Nat Gopalswamy, Emilia Kilpua
Figure caption: In situ observations of the total magnetic field (top panel) and the speed (bottom panel) of the solar wind as obtained from STEREO-A during the ICME Event 5. The two red solid lines mark the boundary of the MC. The cyan arrow marks the HSS following the MC.
Paper: Modeling the Magnetic Vectors of Interplanetary Coronal Mass Ejections at Different Heliocentric Distances with INFROS
Authors: Ranadeep Sarkar, Nandita Srivastava, Nat Gopalswamy, Emilia Kilpua
Figure caption: The top and middle panels show the in situ observations of the total magnetic field and the speed of the solar wind, respectively as obtained by STEREO-B during the ICME Event 2. The two red dashed lines mark the boundary of the MC. The bottom panel is the same as the middle panel but plotted for a much wider temporal window of around four months. The two red solid lines in the bottom panel mark the temporal window within which the top and middle panels are plotted. The cyan dashed lines mark the approximate boundaries of the HSS followed by the ICME. The cyan arrows mark the appearance of the same corotating HSS in the previous solar rotations.
Paper: Modeling the Magnetic Vectors of Interplanetary Coronal Mass Ejections at Different Heliocentric Distances with INFROS
Authors: Ranadeep Sarkar, Nandita Srivastava, Nat Gopalswamy, Emilia Kilpua
Figure caption: The black solid lines within the boundary marked by the vertical red lines denote the magnetic vectors (in SCEQ coordinates) of the ICME, which is sequentially observed by VEX and STEREO-A for Event 5. The gray-shaded regions are the model results obtained for Run1. The cyan and magenta colored dashed lines in the right panels denote the model results for Run2 and Run3, respectively.
Paper: Modeling the Magnetic Vectors of Interplanetary Coronal Mass Ejections at Different Heliocentric Distances with INFROS
Authors: Ranadeep Sarkar, Nandita Srivastava, Nat Gopalswamy, Emilia Kilpua
Figure caption: The black solid lines within the boundary marked by the vertical red lines, denote the magnetic vectors (in SCEQ coordinates) of the ICME which is sequentially observed by VEX and STEREO-B for Event 1. The gray-shaded regions are the results obtained from the model predictions. Among these ensemble model results, the one that best fits the magnetic vectors observed by VEX is denoted as a red dashed line in each plot.
Paper: Modeling the Magnetic Vectors of Interplanetary Coronal Mass Ejections at Different Heliocentric Distances with INFROS
Authors: Ranadeep Sarkar, Nandita Srivastava, Nat Gopalswamy, Emilia Kilpua
Figure caption: Propagation of the CME leading edge and the associated HSS at different times of the CME evolution from the Sun to 1 au as viewed on the ecliptic plane. The black dotted lines denote Parker’s spiral. The gray-shaded region shows the HSS associated with the CME. The curved blue lines depict the CME leading edge. The straight blue lines mark the axis of the two legs of the CME assuming the GCS geometry.