adsabs/AstroCLIMB huggingface dataset:
Paper: Heavy-ion Acceleration in 3He-rich Solar Energetic Particle Events: New Insights from Solar Orbiter
Authors: G. M. Mason, I. Roth, N. V. Nitta, R. Bučík, D. Lario, G. C. Ho, R. C. Allen, A. Kouloumvakos, R. F. Wimmer-Schweingruber, J. Rodriguez-Pacheco
Figure caption: Filled red circles: heavy-ion abundances relative to O from 160 to 226 keV nucleon−1 for both events (proton abundances from 226 to 320 keV nucleon−1); dashed blue lines: abundances from (left) a 3He-rich event survey (Mason et al. 2004) and (right) a survey of Si–S–rich 3He-rich events (Mason et al. 2016); orange lines: model calculations of abundances at (left) 3.2 MK and (right) 10 MK (see text for details). All abundances normalized to O = 1.
Paper: Heavy-ion Acceleration in 3He-rich Solar Energetic Particle Events: New Insights from Solar Orbiter
Authors: G. M. Mason, I. Roth, N. V. Nitta, R. Bučík, D. Lario, G. C. Ho, R. C. Allen, A. Kouloumvakos, R. F. Wimmer-Schweingruber, J. Rodriguez-Pacheco
Figure caption:  Q/M ratios (atomic charge/amu) for different major ion species with ionization state shown by the number below each point. The y-axis is arbitrary to separate the species. Lines at 100 K, 500 K, etc. show average ionization state for an equilibrium plasma (Mazzotta et al. 1998; Post et al. 1977). The thick yellow line shows Q/M where acceleration is suppressed due to damping of plasma waves by 4He.
Paper: Heavy-ion Acceleration in 3He-rich Solar Energetic Particle Events: New Insights from Solar Orbiter
Authors: G. M. Mason, I. Roth, N. V. Nitta, R. Bučík, D. Lario, G. C. Ho, R. C. Allen, A. Kouloumvakos, R. F. Wimmer-Schweingruber, J. Rodriguez-Pacheco
Figure caption: Fraction of each element whose Q/M ratio falls below the damped wave region in Figures 7 and 8 vs. temperature. Flattening of some curves at high temperatures is due to neutron-rich minor isotopes: 13C, 22Ne, 25Mg, 26Mg, etc.
Paper: Heavy-ion Acceleration in 3He-rich Solar Energetic Particle Events: New Insights from Solar Orbiter
Authors: G. M. Mason, I. Roth, N. V. Nitta, R. Bučík, D. Lario, G. C. Ho, R. C. Allen, A. Kouloumvakos, R. F. Wimmer-Schweingruber, J. Rodriguez-Pacheco
Figure caption: Left panel: Fe/O vs. Fe ionization state; right panel: 22Ne/20Ne vs. Fe/Mg ratio. Circles are observations from the surveys of Möbius et al. (2000) and Dwyer et al. (2001). Filled circles are impulsive SEP events; open circles are gradual SEP events. Solid blue line shows model calculation with annotations showing temperature in MK. Dashed blue line is ratio from reference population.
Paper: Heavy-ion Acceleration in 3He-rich Solar Energetic Particle Events: New Insights from Solar Orbiter
Authors: G. M. Mason, I. Roth, N. V. Nitta, R. Bučík, D. Lario, G. C. Ho, R. C. Allen, A. Kouloumvakos, R. F. Wimmer-Schweingruber, J. Rodriguez-Pacheco
Figure caption: Upper panel: red filled circles: mass histogram of ions with energies above 100 keV nucleon−1 for 2022 November 9 event. Blue line: histogram of ions 0.15–0.5 MeV nucleon−1 from survey by Mason et al. (2004), normalized to 2022 event Fe peak. Lower panel: 1/ion speed vs. time of arrival from Figure 1 with filled red circles showing arrival times of individual ions with mass >80 amu.
Paper: Heavy-ion Acceleration in 3He-rich Solar Energetic Particle Events: New Insights from Solar Orbiter
Authors: G. M. Mason, I. Roth, N. V. Nitta, R. Bučík, D. Lario, G. C. Ho, R. C. Allen, A. Kouloumvakos, R. F. Wimmer-Schweingruber, J. Rodriguez-Pacheco
Figure caption: Same as Figure 1 for 3He-rich SEP event starting 2023 April 8, except middle panel energy range is 0.2–10 MeV nucleon−1, and bottom panel oblique line is for a path length of 0.29 au.
Paper: Heavy-ion Acceleration in 3He-rich Solar Energetic Particle Events: New Insights from Solar Orbiter
Authors: G. M. Mason, I. Roth, N. V. Nitta, R. Bučík, D. Lario, G. C. Ho, R. C. Allen, A. Kouloumvakos, R. F. Wimmer-Schweingruber, J. Rodriguez-Pacheco
Figure caption: Event-averaged differential energy spectra for the two events. Left panel: 2022 November 9 event showing unusually high Fe exceeding 4He. Right panel: 2023 April 8 event with 3He exceeding protons above ∼400 keV nucleon−1. Both events show H:4He ratios much lower than typical solar energetic particle populations.
Paper: Heavy-ion Acceleration in 3He-rich Solar Energetic Particle Events: New Insights from Solar Orbiter
Authors: G. M. Mason, I. Roth, N. V. Nitta, R. Bučík, D. Lario, G. C. Ho, R. C. Allen, A. Kouloumvakos, R. F. Wimmer-Schweingruber, J. Rodriguez-Pacheco
Figure caption: Mass histograms for C through Fe ions with energies above 150 keV nucleon−1. Left panel: 2022 November 9 event showing mass enhancement of heavy ions typical of 3He-rich events. Right panel: 2023 April 8 mass histogram showing enhancement pattern of relatively rare 3He-rich events rich in Si and S.
Paper: Heavy-ion Acceleration in 3He-rich Solar Energetic Particle Events: New Insights from Solar Orbiter
Authors: G. M. Mason, I. Roth, N. V. Nitta, R. Bučík, D. Lario, G. C. Ho, R. C. Allen, A. Kouloumvakos, R. F. Wimmer-Schweingruber, J. Rodriguez-Pacheco
Figure caption: Same as Figure 7 showing neutron-rich isotopes of Ne, Mg, and Si, which lie below Q/M= 0.5, which is damped by 4He.
Paper: Multi-spacecraft Observations of the 2022 March 25 CME and EUV Wave: An Analysis of Their Propagation and Interrelation
Authors: Alessandro Liberatore, Paulett C. Liewer, Angelos Vourlidas, Carlos R. Braga, Marco Velli, Olga Panasenco, Daniele Telloni, Salvatore Mancuso
Figure caption: Evolution of the front of the EUV wave in time (left) and space (right). Different colors are different values of position angle (PA): red ≈0°, light blue ≈90°, green ≈180°, and orange ≈270°. The plot on the left shows the distance in time of the EUV front for different PAs. The right image shows the front projected on an EUVI-195 image at a fixed time. The black lines show the considered PAs (36 points separated by 10° each) to outline the front. The error bars are evaluated by performing several times the same process and then evaluating a standard deviation on the measured distances. Negative slopes in the plot indicate a wave reflection. The difficulty in observing the EUV wave at λ = 174 Å does not allow a similar study with the FSI images. However, the black plus symbols give a qualitative idea of the front position as observed by FSI where the wave is more visible (PA ≈220°). A type II radio burst is observed in the range of time delimited by the two dotted vertical lines. The slope of the black line shows the velocity of the expanding surface (≈450 km s−1) retrieved by from the radio data analysis (subsection 3.4).
Paper: Multi-spacecraft Observations of the 2022 March 25 CME and EUV Wave: An Analysis of Their Propagation and Interrelation
Authors: Alessandro Liberatore, Paulett C. Liewer, Angelos Vourlidas, Carlos R. Braga, Marco Velli, Olga Panasenco, Daniele Telloni, Salvatore Mancuso
Figure caption: Overview of the EUV wave–CME decoupling. (a) Propagation of the EUV wavefront (as observed by EUVI) in the FSI field of view. (b) Expanding CME as observed by FSI. A huge lateral expansion can be seen by comparing (b.1) and (b.2). The EUV wave is still a driven wave. Moving from (b.2) to (b.3), the CME lateral expansion is almost stopped. We expect to have the decoupling. (c) It is possible to notice the moment of the CME–EUV wave decoupling. Indeed, (c.2) shows two fronts: an inner one (the expanding CME) and an outer one (the EUV wave). (c.2) is the difference between the frames at 05:17:30 and 05:20:00 UTC. The dark blue and blue vertical lines are, respectively, the CME fronts as observed by SolO/FSI in (b.1) and (b.2). Then, from 05:20, the EUV wave is not driven anymore, and we expect to see a decrease in velocity (compare with Figure 6). Finally, (c.3) shows the wave propagating as a fast-mode wave avoiding the high-density regions on the solar east side (Figure 8). Note: the times reported in each frame are in the S/C reference system. To properly compare the wavefront positions observed by STA/EUVI with the CME front positions observed by SolO/FSI, we must consider the light travel time between the two S/C (≈5 minutes, 20 s). For this reason, the closest STA/EUVI frame to the SolO frame at 05:10 is the one at 05:15 UTC.
Paper: Multi-spacecraft Observations of the 2022 March 25 CME and EUV Wave: An Analysis of Their Propagation and Interrelation
Authors: Alessandro Liberatore, Paulett C. Liewer, Angelos Vourlidas, Carlos R. Braga, Marco Velli, Olga Panasenco, Daniele Telloni, Salvatore Mancuso
Figure caption: The 2022 March 25 CME as observed by three instruments on SolO during its first close perihelion (≈0.32 au) at ≈05:00 UTC. (a) Images from FSI (λ = 174 Å) just before the event (a.1, ≈05:00 UTC) and during the first visible CME front (a.2, ≈05:10 UTC). (b) Composite of the FSI-174 image (orange) and the polarized brightness obtained by the Metis coronagraph (gray, λ = 580–640 nm) showing the corona details just before the event (b.1, ≈05:00 UTC) and when the front reached the Metis internal FOV (b.2, ≈05:30 UTC). (c) Composites of FSI-174, Metis, and SoloHI images at ≈06:20, 07:30, 09:10, and 10:45 UTC. SoloHI follows the evolution of the CME at very large heliocentric distances (>55 R ⊙). The CME is clearly visible even after 15:00 UTC. Note: all the Metis and SoloHI images in this figure are a difference of two consecutive images to highlight changes in the complex, evolving CME.
Paper: Multi-spacecraft Observations of the 2022 March 25 CME and EUV Wave: An Analysis of Their Propagation and Interrelation
Authors: Alessandro Liberatore, Paulett C. Liewer, Angelos Vourlidas, Carlos R. Braga, Marco Velli, Olga Panasenco, Daniele Telloni, Salvatore Mancuso
Figure caption: CME and EUV wave (orange arrows) as observed by SolO/FSI-174. Each image is the difference between two consecutive frames. Due to the different wavelength, the EUV wave is not as clearly visible as in STA/EUVI-195. However, it is possible to clearly observe the front of the CME in its early stage (not visible by either STEREO-A or SOHO). The times reported in each frame are in the SolO reference system. To properly compare the wavefront positions observed by SolO with the wavefront positions observed by STEREO-A, we must consider the light travel time between the two S/C. Thus, each SolO frame acquired at a time T must be compared with the STEREO-A frame at T + 5 minutes, 20 s.
Paper: Multi-spacecraft Observations of the 2022 March 25 CME and EUV Wave: An Analysis of Their Propagation and Interrelation
Authors: Alessandro Liberatore, Paulett C. Liewer, Angelos Vourlidas, Carlos R. Braga, Marco Velli, Olga Panasenco, Daniele Telloni, Salvatore Mancuso
Figure caption: Relative position of the S/C on 2022 March 25 at 05:00:00 am UTC (Gieseler et al. 2023). STEREO-A (red square) and SolO (blue square) are near quadrature.
Paper: Heavy-ion Acceleration in 3He-rich Solar Energetic Particle Events: New Insights from Solar Orbiter
Authors: G. M. Mason, I. Roth, N. V. Nitta, R. Bučík, D. Lario, G. C. Ho, R. C. Allen, A. Kouloumvakos, R. F. Wimmer-Schweingruber, J. Rodriguez-Pacheco
Figure caption: Enhancement of ions vs. Q/M compared to gradual SEP events and solar system abundances (above Fe). Red points from Mason et al. (2004) survey; blue points from 2022 November 9 event. Fitted slope of power-law fit to red points is −3.26.
Paper: Multi-spacecraft Observations of the 2022 March 25 CME and EUV Wave: An Analysis of Their Propagation and Interrelation
Authors: Alessandro Liberatore, Paulett C. Liewer, Angelos Vourlidas, Carlos R. Braga, Marco Velli, Olga Panasenco, Daniele Telloni, Salvatore Mancuso
Figure caption: CME as observed by STA/COR2 (left) and SOHO/LASCO-C2 (right). The two S/C were separated by about 33°.
Paper: Detecting Technosignatures from Earth-scale Civilizations
Authors: Reza Ashtari
Figure caption: A visualization for the effect of signal beamwidth and pointing on signal reception. All subfigures assume an antenna diameter of 70 m, 70% antenna efficiency, 100 kW of RF transmit power, and distance of 10 lt-yr. The transmission source is shown as a red circle, the Sun is shown as a yellow circle, and the white outline of the transmitted beam represents the detectable level of flux (the 1σ sensitivity limit of the VLA is shown in this example). If the Sun is within the white detection envelope, then enough flux from the technosignature reaches Earth for successful measurement. Top left: visualization of a 1 GHz transmission and the standard DSN pointing error of ∼0.°004 (NASA 2017; Slobin & Pham 2013); bottom left: a 1 GHz transmission with a pointing error of 0.°104; top right: a 10 GHz transmission with a pointing error of 0.°004°; and bottom right: a 10 GHz transmission with a pointing error of 0.°104. The key takeaway from this figure is that given a fixed value for how large of an antenna is available, higher-frequency operations enable the use of more directive and narrow beamwidths but also demand more precise beam steering as a result. Unless a civilization is intentionally directing transmissions toward Earth, lower-frequency observations are significantly favored. This relationship between the flux at Earth from misaligned Earth-scale technosignatures vs the sensitivities of observatories is presented in Figure 9.
Paper: Detecting Technosignatures from Earth-scale Civilizations
Authors: Reza Ashtari
Figure caption: Time duration of beamed emission from a fixed transmit antenna on an exoplanet with a 1 day rotation period. Values assume a frequency of 1 GHz. Blue lines represent how long a transmission would illuminate Earth based on the size of the transmit antenna. Orange lines represent how long a transmission would illuminate Earth based on the transmission’s half-power beamwidth. The windowed plot shows the same information on a timescale of 5 minutes, highlighting the shorter observational periods for transmissions from fixed antennas (transmitted without the use of a tracking or active pointing system). For example, a 1000 m2 aperture, transmitting from a fixed antenna at 1 GHz on a planet with a rotation period of 1 day, could not illuminate the Earth for greater than 2 minutes unless a tracking mechanism or mount is used. This shortcoming of fixed antennas relative to interplanetary communications and radar justifies why beam-tracking is a crucial component in detecting any directive deep space transmissions. These plots further highlight the temporal benefit of pursuing tracked, interplanetary communications and radar operations with well-defined, hours-long observation windows about secondary eclipses and PPOs.
Paper: Detecting Technosignatures from Earth-scale Civilizations
Authors: Reza Ashtari
Figure caption: Effect of angular misalignment on narrowband signal detection. This figure assumes an Earth-scale deep space communications uplink transmission (70 m antenna diameter, 100 kW RF  transmission power) at a distance of 10 lt-yr from Earth. For these fixed assumptions in antenna size and transmission power, it is clear to see the increasing difficulty for tolerating misalignment when using narrower beamwidths at higher frequencies. Thus, for eavesdropping scenarios where transmissions are not intentionally directed toward Earth, lower-frequency observations should be prioritized before those of higher frequencies.
Paper: Detecting Technosignatures from Earth-scale Civilizations
Authors: Reza Ashtari
Figure caption: Detectability of exoplanetary narrowband communications (70 m antenna diameter, 100 kW of RF transmission power, 0.005°(18″) pointing accuracy). Observatory sensitivities are calculated using Equation (B3), assuming measurement across two polarizations, and a 3 Hz receiver channel bandwidth (standard for Breakthrough Listen radio receivers; Enriquez et al. 2017). The takeaway of this is that for the foreseeable future, no current or planned radio observatory will be able to even detect a narrowband technosignature from greater than 100 lt-yr, unless the transmission is beyond NASA’s current deep space communication capabilities (NASA 2017).
Paper: Detecting Technosignatures from Earth-scale Civilizations
Authors: Reza Ashtari
Figure caption: Detectability of exoplanetary wideband radar signals (70 m antenna diameter, 1 MW of RF transmission power, 0.005°(18″) pointing accuracy). Observatory sensitivities are calculated using Equation (B2). Sensitivity values of 1σ assume measurements across two polarizations and 108 samples (τ intΔv = 108 samples). As shown in Table 2 and illustrated in Figure 12, these high-powered wideband signals feasibly provide our observatories with greater search radii but are not as predictable, prevalent, or persistent as narrowband interplanetary communications relative to Earth’s recent history of deep space transmissions (Mudgway 2001).
Paper: Detecting Technosignatures from Earth-scale Civilizations
Authors: Reza Ashtari
Figure caption: The approach for selecting observation windows is shown above. Top: first, the elevation angle of the target is plotted. A dashed horizontal black line is shown to display the cutoff elevation angle for observations. Twenty degrees is selected here as the elevation limit, per common practice (NASA 2017; Braun et al. 2015). Middle: next, the orbital phase of the targeted exoplanet is evaluated over the same time period. Here, it is assumed an orbital phase of 0 is equal to the time of transit center or when the planet is between the star and our view from Earth. For observing secondary eclipses, we want to observe when the planet is behind its star, so when the orbital phase is equal to 0.5. To observe the period before, through, and after the secondary eclipse, we designate orbital phases from 0.45 to 0.55 to be of interest. Bottom: finally, cross-referencing the periods when the elevation of the target is greater than 20° and the orbit of the targeted planet is in the correct phase, we show the observational windows meeting our criteria. Each observational period/visit is shown in a different color. Data shown in these three figures are generated using the astroplan Python software package (Morris et al. 2018).
Paper: Detecting Technosignatures from Earth-scale Civilizations
Authors: Reza Ashtari
Figure caption: Geometry for observing interplanetary communications to a planetary orbiter before and after interplanetary conjunctions. Note this configuration also applies for observing interplanetary radar.
Paper: Detecting Technosignatures from Earth-scale Civilizations
Authors: Reza Ashtari
Figure caption: Geometry for observing interplanetary communications to a stellar orbiter before and after secondary eclipses.
Paper: Detecting Technosignatures from Earth-scale Civilizations
Authors: Reza Ashtari
Figure caption: Cumulative number of exoplanets discovered for all discovery methods vs. year (Courtesy of NASA Exoplanet Archive 2022).
Paper: Detecting Technosignatures from Earth-scale Civilizations
Authors: Reza Ashtari
Figure caption: Illustration of down-selecting candidate exoplanets based on the range limits of an observatory. The ATCA is used as an example, with its maximum range limits (from Table 2) plotted against candidate exoplanets. While no exoplanets are within the ATCA’s detection radius for narrowband Earth-scale technosignatures (red), several candidate exoplanets are within the ATCA’s range limit for wideband interplanetary radar-like technosignatures (purple). The global ESI for each candidate exoplanet is depicted using the color bar, where green represents an ESI closer to 1.0 (more similar to Earth). This down-selection process is repeated for all observatories and exoplanets of interest, the results of which are shown in Table 3.
Paper: Shocks Power Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble, Mark Avara
Figure caption: The density distribution around the BH excision (yellow dot) in the equatorial plane at four different times, t/t 0 = 0.5, 1, 2, and 3. The extent of the inset is 500r g.
Paper: Shocks Power Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble, Mark Avara
Figure caption: Successive moments in a full TDE simulated using two domains: the density distribution of the star before (1) and after (2) the pericenter passage, and the debris after the pericenter passage (3 and 4) in the equatorial plane. The yellow dot in the big left panel indicates the BH. The cyan boxes in the four right panels depict the boundary of Domain1. Once the star is disrupted, we increase the size of the box (from 2 to 3) to keep the debris inside Domain1, where the self-gravity is calculated as much as possible. The panels are not drawn to scale.
Paper: Shocks Power Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble, Mark Avara
Figure caption: The mass fallback rate ﹩\dot{M}﹩, using the energy distribution shown in Figure 2. The rate and time are normalized by ﹩{\dot{M}}_{0}={M}_{\star }/3{t}_{0}﹩ and t 0, respectively. The horizontal dashed line indicates the Eddington limit with radiative efficiency of 0.01 and the diagonal dashed line a power law of t −5/3.
Paper: Shocks Power Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble, Mark Avara
Figure caption: The energy distribution of debris at t ≃ 0.4t 0. The vertical dashed line (E/Δϵ = Ξ ≃ −1.64) shows the characteristic energy at which the fallback rate peaks (see Figure 3).
Paper: Detecting Technosignatures from Earth-scale Civilizations
Authors: Reza Ashtari
Figure caption: Earth similarity of the interiors and surfaces of surveyed exoplanets, with 0 being less Earth-like and 1 being more Earth-like.
Paper: Detecting Technosignatures from Earth-scale Civilizations
Authors: Reza Ashtari
Figure caption: Earth similarity scores for the (top left) planetary radius, (top right) density, (bottom left) escape velocity, and (bottom right) surface temperature of surveyed exoplanets, with 0 being less Earth-like and 1 being more Earth-like.
Paper: Detecting Technosignatures from Earth-scale Civilizations
Authors: Reza Ashtari
Figure caption: Region plausible for detecting technosignatures. The area for which we can search for Earth-scale technosignatures (red circle) is shown in scale against the galaxy for reference.
Paper: Shocks Power Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble, Mark Avara
Figure caption: The location of the thermalization photosphere (magenta curves) as seen by a distant observer plotted over the density distribution at ϕ = 0 at t/t 0 = 1, 2, and 3 (top panels) and at ϕ = 90°, 180◦, and 270◦ at t/t 0 = 3 (bottom panels). We define the thermalization optical depth as ﹩\sqrt{{\tau }_{{\rm{t}}}{\tau }_{\mathrm{ff}}}﹩, for τ T (τ ff) the Thomson (absorption) optical depths integrated radially inward from the outer boundary.
Paper: Shocks Power Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble, Mark Avara
Figure caption: The mass-weighted average of the specific orbital energy of debris (top left), angular momentum (top right), eccentricity (bottom left), and aspect ratio (bottom right) for given r at t/t 0 = 0.5, 1, 2, and 3. The dashed gray vertical lines in all panels indicate the pericenter distance of the original stellar orbit. The dotted gray horizontal lines in some panels show different quantities: E = Δϵ (top left), initial angular momentum (top right), and R ⋆/r p (bottom right). The diagonal black line in the top left panel shows a power law of r −1.
Paper: Shocks Power Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble, Mark Avara
Figure caption: Accumulated mass normalized by M ⋆ as a function of the distance from the SMBH at t/t 0 ≃ 0.5, 1, 2, and 3. The dashed black vertical line indicates the pericenter distance of the original stellar orbit. The mass expelled through the radial inner boundary at r = 40r g is included as if the accreted mass is confined within r = 40r g.