adsabs/AstroCLIMB huggingface dataset:
Paper: Ground-based Observations of Temporal Variation of the Cosmic-Ray Spectrum during Forbush Decreases
Authors: W. Mitthumsiri, D. Ruffolo, K. Munakata, M. Kozai, Y. Hayashi, C. Kato, P. Muangha, A. Sáiz, P. Evenson, P.-S. Mangeard, J. Clem, S. Seunarine, W. Nuntiyakul, N. Miyashita, R. Kataoka, A. Kadokura, S. Miyake, K. Iwai, H. Menjo, E. Echer, A. Dal Lago, M. Rockenbach, N. J. Schuch, J. V. Bageston, C. R. Braga, H. K. Al Jassar, M. M. Sharma, N. Burahmah, F. Zaman, M. L. Duldig, I. Sabbah, T. Kuwabara
Figure caption: Temporal variations of cosmic-ray flux ΔI(P, t) (left) and spectral index ΔΓ(P, t) (right) relative to a reference interval (first 3 days of each plot), based on two ground-based observing techniques, GFA (red) and South Pole L (blue) (hourly data: thin, light curves; 24 hr running averages: thick, dark curves) and, when available, space-based daily AMS-02 proton data (black). Each panel displays values for rigidity 10.5 GV during 27 day solar rotation periods including five FDs starting in (a) 2015 March, (b) 2015 June, (c) 2017 September, (d) 2021 November, and (e) 2023 November. FDs are associated with interplanetary shock arrival at Earth (vertical line) and/or passage of an ICME (shading of the same color). There is very good consistency between all measures of GCR flux and spectral variations. Two GLEs (solar energetic particle enhancements) in (c) 2017 September and (d) 2021 October were observed by ground-based detectors but excluded from published AMS-02 data.
Paper: Ground-based Observations of Temporal Variation of the Cosmic-Ray Spectrum during Forbush Decreases
Authors: W. Mitthumsiri, D. Ruffolo, K. Munakata, M. Kozai, Y. Hayashi, C. Kato, P. Muangha, A. Sáiz, P. Evenson, P.-S. Mangeard, J. Clem, S. Seunarine, W. Nuntiyakul, N. Miyashita, R. Kataoka, A. Kadokura, S. Miyake, K. Iwai, H. Menjo, E. Echer, A. Dal Lago, M. Rockenbach, N. J. Schuch, J. V. Bageston, C. R. Braga, H. K. Al Jassar, M. M. Sharma, N. Burahmah, F. Zaman, M. L. Duldig, I. Sabbah, T. Kuwabara
Figure caption: (a) Daily mean ΔI10.5 versus rigidity observed by AMS-02 (black) and by GFA (red) on 2015 June 25, a time of maximum FD. (b) ΔI10.5 versus rigidity observed by AMS-02 (black) during 2015 April 15 to May 11 at solar maximum relative to 2019 October 18 to November 13 during solar minimum. At P ≳ 7 GV, both types of changes can be described by a power-law deficit, while at lower rigidity, the spectral changes of FDs and solar modulation are different.
Paper: Satellite Formation around the Largest Asteroids
Authors: Kevin J. Walsh, Ronald-Louis Ballouz, Harrison F. Agrusa, Josef Hanus̆, Martin Jutzi, Patrick Michel
Figure caption: Evolution of the target asteroid immediately following impact. The outcome of a 13 km object impacting a 100 km spherical target with a 4 hr preimpact rotation at a 60∘ angle at a speed of 5 km s−1 shown at 0.1, 1, 3, 5, 7, and 9 hr post-impact. The particles that are part of the main primary mass are colored gray. The rest of the particles are colored by the pericenter of their instantaneous Keplerian orbit. Red colors correspond to trajectories with a pericenter less than the primary’s long axis, while blue colors indicate pericenters above the primary’s long axis. Dark red indicates a pericenter less than zero, which corresponds to a hyperbolic (unbound) orbit.
Paper: Satellite Formation around the Largest Asteroids
Authors: Kevin J. Walsh, Ronald-Louis Ballouz, Harrison F. Agrusa, Josef Hanus̆, Martin Jutzi, Patrick Michel
Figure caption: Evolution of the target asteroid immediately following impact. The outcome of a 13 km object impacting a 100 km spherical target with no rotation at a 60∘ angle at a speed of 5 km s−1 shown at 0.1, 1, 3, 5, 7, and 9 hr post-impact. The particles that are part of the main primary mass are colored gray. The rest of the particles are colored by the pericenter of their instantaneous Keplerian orbit. Red colors correspond to trajectories with a pericenter less than the primary’s long axis, while blue colors indicate pericenters above the primary’s long axis. Dark red indicates a pericenter less than zero, which corresponds to a hyperbolic (unbound) orbit.
Paper: Satellite Formation around the Largest Asteroids
Authors: Kevin J. Walsh, Ronald-Louis Ballouz, Harrison F. Agrusa, Josef Hanus̆, Martin Jutzi, Patrick Michel
Figure caption: The outcome of a 5 km s−1 impact of a 10 m impactor into a 1 km target with different preimpact rotation states. All images are following the handoff from SPH to pkdgrav. (a) A nonspinning target results in a moderately prolate object with minimal spin (see Figure 9 for the evolution of the spin rate of the largest remnant). (b) An SPH simulation with the target initially spinning at 6 hr. (c) The same impact with the spin adjusted to apply 6 hr preimpact rotation on the target 100 s after impact.
Paper: Satellite Formation around the Largest Asteroids
Authors: Kevin J. Walsh, Ronald-Louis Ballouz, Harrison F. Agrusa, Josef Hanus̆, Martin Jutzi, Patrick Michel
Figure caption: Provenance of satellites. The provenance of all temporary satellites (black circles) and temporary satellites with pericenters greater than 1.5Rpri (purple) for six different simulation outcomes are used to shown the normalized mass originating from different depths of the target. The solid gray line is the distribution of all mass in the parent body, and all curves are normalized to show the relative preference for satellite provenance.
Paper: Satellite Formation around the Largest Asteroids
Authors: Kevin J. Walsh, Ronald-Louis Ballouz, Harrison F. Agrusa, Josef Hanus̆, Martin Jutzi, Patrick Michel
Figure caption: The outcome of a 5 km s−1 impact of a 10 m impactor into a 1 km target with different preimpact rotation states. (a) The axis ratio c/a of the largest remnant as a function of time for all three cases. (b) The rotation period of the largest remnant for the 6 hr impact case and the applied 6 hr rotation case (the nonspinning target case converged to 114 hr and is not shown). (c) The number of N-body particles in the largest remnant over time since impact for all three cases.
Paper: Satellite Formation around the Largest Asteroids
Authors: Kevin J. Walsh, Ronald-Louis Ballouz, Harrison F. Agrusa, Josef Hanus̆, Martin Jutzi, Patrick Michel
Figure caption: Temporary satellites plotted in gray on a color scale of dynamical lifetimes as a function of orbital eccentricity and pericenter distance. The impact properties for each case can be found in Table 1.
Paper: ODIN: Star Formation Histories Reveal Formative Starbursts Experienced by Lyα-emitting Galaxies at Cosmic Noon
Authors: Nicole M. Firestone, Eric Gawiser, Kartheik G. Iyer, Kyoung-Soo Lee, Vandana Ramakrishnan, Francisco Valdes, Changbom Park, Yujin Yang, Anahita Alavi, Robin Ciardullo, Norman Grogin, Caryl Gronwall, Lucia Guaita, Sungryong Hong, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Anton M. Koekemoer, Ankit Kumar, Jaehyun Lee, Vihang Mehta, Gautam Nagaraj, Julie Nantais, Laura Prichard, Marc Rafelski, Hyunmi Song, Ben Sunnquist, Harry I. Teplitz, Xin Wang
Figure caption: Examples of three classes of observed LAE SFHs and their SED fits: first burst, dominant burst, and nondominant burst. Each LAE used in this figure has a confirmed spectroscopic redshift. In each SFH (top), the x-axis represents the lookback time in Gyr, and the y-axis represents the SFR as a function of time in M⊙ yr−1. The black solid line represents the median Dense Basis SFHs. The gray shaded region represents the 25%–75% confidence interval for the SFH. The blue shaded region represents the last 200 Myr, i.e., the age range of stars able to dominate the rest-UV light at the time of observation. The red solid vertical line represents the time at which the galaxy reached its maximum SFR. In cases where the maximum SFR occurs “now” (in the last 200 Myr), it is highlighted in yellow. In each SED fit (bottom), the x-axis represents the wavelength λ in angstroms, and the y-axis represents the flux density Fν in μJy. The blue points represent the photometric data, and the black lines represent the spectral template models used to determine the median SFH and confidence intervals in the above panels.
Paper: ODIN: Star Formation Histories Reveal Formative Starbursts Experienced by Lyα-emitting Galaxies at Cosmic Noon
Authors: Nicole M. Firestone, Eric Gawiser, Kartheik G. Iyer, Kyoung-Soo Lee, Vandana Ramakrishnan, Francisco Valdes, Changbom Park, Yujin Yang, Anahita Alavi, Robin Ciardullo, Norman Grogin, Caryl Gronwall, Lucia Guaita, Sungryong Hong, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Anton M. Koekemoer, Ankit Kumar, Jaehyun Lee, Vihang Mehta, Gautam Nagaraj, Julie Nantais, Laura Prichard, Marc Rafelski, Hyunmi Song, Ben Sunnquist, Harry I. Teplitz, Xin Wang
Figure caption: SFHs of z = 2.4 LAEs. The specifications in this figure match those of the SFHs in Figure 1. Plots outlined in green highlight LAEs with spectroscopic confirmations. The green and pink vertical lines (when present) represent the lookback times corresponding to z = 3.1 and 4.5, respectively. In this sample, there are 24 LAEs with first burst SFHs, five LAEs with a dominant burst SFH, and two LAEs with nondominant burst SFHs.
Paper: ODIN: Star Formation Histories Reveal Formative Starbursts Experienced by Lyα-emitting Galaxies at Cosmic Noon
Authors: Nicole M. Firestone, Eric Gawiser, Kartheik G. Iyer, Kyoung-Soo Lee, Vandana Ramakrishnan, Francisco Valdes, Changbom Park, Yujin Yang, Anahita Alavi, Robin Ciardullo, Norman Grogin, Caryl Gronwall, Lucia Guaita, Sungryong Hong, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Anton M. Koekemoer, Ankit Kumar, Jaehyun Lee, Vihang Mehta, Gautam Nagaraj, Julie Nantais, Laura Prichard, Marc Rafelski, Hyunmi Song, Ben Sunnquist, Harry I. Teplitz, Xin Wang
Figure caption: Total stellar mass histograms for three SFH archetypes of LAEs and LBGs at each redshift. The columns represent z = 2.4 (left), 3.1 (middle), and 4.5 (right). The rows represent the first burst (upper), dominant burst (middle), and nondominant burst (lower) archetypes. In each histogram, the x-axis represents the log of the total stellar mass M* in solar masses. The y-axis represents the number of galaxies Ngal. The blue histograms represent the LAEs, and the pink histograms represent the LBGs, with the open pink histograms denoting random samples of 30 high stellar mass LBGs that were not included in the LBG control sample.
Paper: ODIN: Star Formation Histories Reveal Formative Starbursts Experienced by Lyα-emitting Galaxies at Cosmic Noon
Authors: Nicole M. Firestone, Eric Gawiser, Kartheik G. Iyer, Kyoung-Soo Lee, Vandana Ramakrishnan, Francisco Valdes, Changbom Park, Yujin Yang, Anahita Alavi, Robin Ciardullo, Norman Grogin, Caryl Gronwall, Lucia Guaita, Sungryong Hong, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Anton M. Koekemoer, Ankit Kumar, Jaehyun Lee, Vihang Mehta, Gautam Nagaraj, Julie Nantais, Laura Prichard, Marc Rafelski, Hyunmi Song, Ben Sunnquist, Harry I. Teplitz, Xin Wang
Figure caption: SFHs of z = 4.5 LAEs. The specifications in this figure match those of the SFHs in Figure 1. In this sample, there are 13 LAEs with first burst SFHs, seven LAEs with dominant burst SFHs, and two LAEs with nondominant burst SFHs.
Paper: ODIN: Star Formation Histories Reveal Formative Starbursts Experienced by Lyα-emitting Galaxies at Cosmic Noon
Authors: Nicole M. Firestone, Eric Gawiser, Kartheik G. Iyer, Kyoung-Soo Lee, Vandana Ramakrishnan, Francisco Valdes, Changbom Park, Yujin Yang, Anahita Alavi, Robin Ciardullo, Norman Grogin, Caryl Gronwall, Lucia Guaita, Sungryong Hong, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Anton M. Koekemoer, Ankit Kumar, Jaehyun Lee, Vihang Mehta, Gautam Nagaraj, Julie Nantais, Laura Prichard, Marc Rafelski, Hyunmi Song, Ben Sunnquist, Harry I. Teplitz, Xin Wang
Figure caption: SFHs of z = 3.1 LAEs. The specifications in this figure match those of the SFHs in Figure 1. In this sample, there are 12 LAEs with first burst SFHs and nine LAEs with dominant burst SFHs.
Paper: Ground-based Observations of Temporal Variation of the Cosmic-Ray Spectrum during Forbush Decreases
Authors: W. Mitthumsiri, D. Ruffolo, K. Munakata, M. Kozai, Y. Hayashi, C. Kato, P. Muangha, A. Sáiz, P. Evenson, P.-S. Mangeard, J. Clem, S. Seunarine, W. Nuntiyakul, N. Miyashita, R. Kataoka, A. Kadokura, S. Miyake, K. Iwai, H. Menjo, E. Echer, A. Dal Lago, M. Rockenbach, N. J. Schuch, J. V. Bageston, C. R. Braga, H. K. Al Jassar, M. M. Sharma, N. Burahmah, F. Zaman, M. L. Duldig, I. Sabbah, T. Kuwabara
Figure caption: Daily South Pole NM leader fraction L versus AMS-02 Γ10.5 (cosmic-ray spectral index at 10.5 GV). Blue squares: the two FD periods in 2015. Red circles: all other data during 2015–2019, indicating variation with the solar activity cycle. Slopes of linear fits to the two data sets are 20.4 ± 0.2 (red) and 30.7 ± 1.8 (blue).
Paper: Satellite Formation around the Largest Asteroids
Authors: Kevin J. Walsh, Ronald-Louis Ballouz, Harrison F. Agrusa, Josef Hanus̆, Martin Jutzi, Patrick Michel
Figure caption: The population of observed large asteroids with satellites. (a) The size ratio of satellites to primary body as a function of their orbit semimajor axis scaled by the primary radii for the observed population of satellites among asteroids with diameter greater than 100 km. Multiple systems are connected with lines, and the size of each point gives a relative scale of the size of the primary, where D = 286 km (87) Sylvia is indicated for scale. (b) Rotation periods of asteroids larger than 50 km as a function of diameter derived from light-curve observations, where S-complex and C-complex objects are in red and blue, respectively, and those with observed satellites are aqua. (c) Asteroid light-curve amplitudes in magnitude plotted as a function of the asteroid’s rotation period in hours, where all asteroids are in purple and those with satellites are in aqua. The light-curve amplitudes are from the same light-curve database and can be roughly translated into axis ratios via ﹩{\rm{\Delta }}m=2.5\mathrm{log}(a/b)﹩, where Δm is the light-curve amplitude and a and b are the long and intermediate principal axes, respectively.
Paper: Satellite Formation around the Largest Asteroids
Authors: Kevin J. Walsh, Ronald-Louis Ballouz, Harrison F. Agrusa, Josef Hanus̆, Martin Jutzi, Patrick Michel
Figure caption: Two different impact outcomes with similar post-impact shape and total mass lost, but with different post-impact spin rates, where (a) a case resulting in a mildly elongated final shape (a, b, c = 57, 45, 40 km) but rapid 6.7 hr rotation period places numerous initial satellites into the medium-term stable regions (satellites plotted as gray circles). The impact scenario had a 13 km impactor hit at an oblique 60∘ impact angle into an initially 10 hr rotating target that resulted in 80% of the mass remaining in the largest remnant (case 17 in Table 1). (b) An outcome with a similarly elongated final shape (a, b, c = 59, 52, 34 km) but a final 12.2 hr rotation period that resulted in nearly all initial orbits having pericenters below 1 primary radius and almost certain to reimpact. The impactor was 7 km and impacted at a 45∘ angle, resulting in a final remnant with 88% of the total system mass (Case 12 in Table 1). The diagonal structures on these plots are locations of constant semimajor axis and correspond to spin–orbit resonances with the primary.
Paper: Satellite Formation around the Largest Asteroids
Authors: Kevin J. Walsh, Ronald-Louis Ballouz, Harrison F. Agrusa, Josef Hanus̆, Martin Jutzi, Patrick Michel
Figure caption: Evolution of the target asteroid immediately following impact. The outcome of a 13 km object impacting a 100 km spherical target with a 10 hr preimpact rotation at a 60∘ angle at a speed of 5 km s−1 shown at 0.1, 1, 3, 5, 7, and 9 hr post-impact. The particles that are part of the main primary mass are colored gray. The rest of the particles are colored by the pericenter of their instantaneous Keplerian orbit. Red colors correspond to trajectories with a pericenter less than the primary’s long axis, while blue colors indicate pericenters above the primary’s long axis. Dark red indicates a pericenter less than zero, which corresponds to a hyperbolic (unbound) orbit. See Figures 11 and 12 in the Appendix for visualizations of the same impact with a nonspinning target and a target initially with a 4 hr rotation period, respectively.
Paper: Satellite Formation around the Largest Asteroids
Authors: Kevin J. Walsh, Ronald-Louis Ballouz, Harrison F. Agrusa, Josef Hanus̆, Martin Jutzi, Patrick Michel
Figure caption: Properties of temporary satellites from simulation outcomes. The normalized mass of satellites having initial orbits with pericenters above 1 primary long semiaxis length as a function of (a) primary post-impact axis ratio a/b, (b) primary post-impact rotation period, (c) mass of the largest remnant mass as a fraction of the total system mass (including escaping material), and (d) the ratio of the impact energy to the rotation-dependent catastrophic disruption threshold. The size of each point represents the total number of temporary satellites for each given simulation where the numbers spanned 0–316. The normalized mass is the total mass in satellites as a fraction of the primary’s mass. The gray zone in panel (b) shows the spin rates for all known primaries in the observed sample.
Paper: Satellite Formation around the Largest Asteroids
Authors: Kevin J. Walsh, Ronald-Louis Ballouz, Harrison F. Agrusa, Josef Hanus̆, Martin Jutzi, Patrick Michel
Figure caption: The fates of test particles in orbit around an ellipsoidal primary as a function of its bulk density and spin period. The primary has the same semiaxis lengths as those from Figures 5(a) and 6 (a, b, c ∼ 57, 45, 40 km), and the top row shows the same simulations as plotted in Figure 6. The black line indicates the semimajor axis corresponding to the synchronous orbit. Orbits below this line would tidally evolve inward owing to tides. In general, as the primary’s density or spin period is increased, the periods of close-in orbits become closer to the primary’s spin period, leading to smaller stable regions owing to the stronger perturbing effect of C22.
Paper: Satellite Formation around the Largest Asteroids
Authors: Kevin J. Walsh, Ronald-Louis Ballouz, Harrison F. Agrusa, Josef Hanus̆, Martin Jutzi, Patrick Michel
Figure caption: Stability maps for different spin periods. Stability maps are shown as a function of rotation period around a primary with a bulk density of 1 g cm−3 having the same semiaxes as the primary of Figure 5(a) (a, b, c ∼ 57, 45, 40 km) corresponding to a J2 and C22 of ∼0.05 and ∼0.026 when normalized to the primary’s long axis. At short rotation periods, the primary spins much faster than the test particles’ orbit periods, and the perturbing effect of C22 is relatively weak. As the rotation period increases, close-in orbits have shorter lifetimes and the region containing long-term stable orbits is smaller. The colors show the particle lifetime.
Paper: Satellite Formation around the Largest Asteroids
Authors: Kevin J. Walsh, Ronald-Louis Ballouz, Harrison F. Agrusa, Josef Hanus̆, Martin Jutzi, Patrick Michel
Figure caption: Distribution of initial pericenters for temporary satellites. The distribution of satellite pericenters is shown in blue for a nonspinning target hit at an impact angle of 15∘, where all temporary satellites have initial pericenters below 1 primary radius. This contrasts with a target with moderate spin of 10 hr and a highly oblique impact angle of 60∘, shown in red (the same case as shown in Figure 2), that has significant ejecta on orbits with pericenter above 1 and even above 2 primary long semiaxis lengths.
Paper: High-resolution Observations of a C9.3 White-light Flare and Its Impact on the Solar Photosphere
Authors: Zhe Xu, Xiaoli Yan, Zhentong Li, Liheng Yang, Zhike Xue, Jincheng Wang, Yian Zhou
Figure caption: Panels (a)–(c): intensity enhancement maps of the NVST TiO, HMI continuum, and CHASE continuum emissions during the white-light flare. Panels (d) and (e): NVST TiO image and HMI magnetogram illustrating the fine structures of the sunspots and their associated magnetic fields in the flaring region. The three colored contours in panel (e) correspond to enhancement levels of 3%, 8%, and 20% in the respective intensity enhancement maps. Panel (f): ASO-S HXI CLEAN-reconstructed map showing X-ray emission in the 14–20 keV range between 06:00:46 and 06:01:20 UT, coinciding with the occurrence of white-light emission. The white and gray contours outline the umbra and penumbra boundaries of sunspots in the NVST TiO image. Panel (g): light curves of the NVST TiO, HMI continuum, and CHASE continuum emissions integrated over the white dashed box region in panels (a)–(c), respectively. The GOES soft X-ray flux and its time derivative are overplotted in arbitrary units for comparison. Panel (h): light curves of the K1, K2, and FB regions integrated over the orange, yellow, and cyan boxes in NVST TiO images, respectively. The light curves of the AIA 304 Å and NVST Hα integrated over the white dashed box region in Figures 3(h) and (k) are overplotted in arbitrary units for comparison. The labeled times denote the peak times of each curve. The error bars for each curve are the standard deviation of the intensity change taken from the nonflare region (white box in Figure 1(c)).
Paper: High-resolution Observations of a C9.3 White-light Flare and Its Impact on the Solar Photosphere
Authors: Zhe Xu, Xiaoli Yan, Zhentong Li, Liheng Yang, Zhike Xue, Jincheng Wang, Yian Zhou
Figure caption: Panels (a)–(c): AIA 171 Å, 1600 Å, and CHASE continuum images showing the flare SOL2023-09-11T06:01 in AR 13431. The insets in panels (b) and (c) highlight the flare within the active region characterized by a δ-type magnetic configuration. The orange and cyan contours outline the flare brightenings observed in the AIA 1600 Å and CHASE continuum images, respectively. The white box in panel (c) marks the quiet-Sun region, which is used in Figure 2 to normalize the photospheric radiation, as well as to calculate the uncertainties in each light curve. Panel (d): light curves of GOES soft X-ray 1–8 Å flux, its time derivative, and the ASO-S/HXI HXR fluxes corresponding to the white-light flare. Panel (e): HXI HXR background-subtracted count spectrum (black curve) fitted using a combination of a thermal (green curve) and a nonthermal thick target model (yellow curve) at the peak time of the HXR emission. Two vertical dashed lines mark the energy range (11–40 keV) used for the spectral fitting.
Paper: High-resolution Observations of a C9.3 White-light Flare and Its Impact on the Solar Photosphere
Authors: Zhe Xu, Xiaoli Yan, Zhentong Li, Liheng Yang, Zhike Xue, Jincheng Wang, Yian Zhou
Figure caption: Panels (a)–(d): NVST TiO images illustrating the sudden formation of a small pore in the white-light flare region. Panels (e) and (f): photospheric flow fields derived using the optical flow method applied to NVST TiO images, showing the velocity patterns 5 minutes before and after the white-light flare. Panels (g) and (h): maps of the total magnetic field strength before and after the white-light flare, highlighting magnetic field changes in the flare region. The blue and gray contours overlaid in panels (a) and (e)–(h) denote the locations of the white-light flare kernels. The white contour in panel (h) marks the magnetic field amplification region with enhanced strength greater than 150 G.