adsabs/AstroCLIMB huggingface dataset:
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: (a) Depth and (b) velocity of the centroid of each rising MFR in the convection zone as a function of time during their rise. Dashed lines correspond to isothermally buoyant MFRs. The curves are cut off when each MFR emerges, and the corresponding dashed lines are cut off at the same time. The black horizontal line in panel (b) shows the maximum rise velocity of magnetic flux at a depth of 20 Mm as inferred by Birch et al. (2016).
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Cross-sectional cuts of B  y  during the rise of the MFR at several time steps in the y–z plane. From top to bottom, the rows represent ζ = 0, 0.5, 1, and 2.
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Field lines at two different times early in the ζ = 0.5 simulation from above and the side. Red, pink, blue, green, and yellow field lines are traced from the bottom boundary of the simulation domain, at ﹩{s}^{2}={x}^{2}+{(y\pm {r}_{0})}^{2}﹩ for s = 3,  5.5,  7,  9.5, and  12 L 0, respectively. Orange field lines are traced from the upper photosphere. Because the field lines are line-tied at the bottom boundary, in the absence of the reconnection or diffusion, the field lines shown in the figures are the same at each time step (except for the orange ones).
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Cross-sectional cuts of B  y  during the rise of the MFR at several time steps in the x–z plane. From top to bottom, the rows represent ζ = 0, 0.5, 1, and 2.
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption:  B  z  at several different times during the ζ = 0.5 simulation, saturated near the peak value of ∣B  z ∣.
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: The radius–depth evolution of the MFR across the (a) z- and (b) x-directions. Dashed lines are the isothermally buoyant MFRs. The curves are cut off when each MFR emerges.
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Emergence time as a function of twist. The circles represent the simulations set to rise initially at the same speed. The boxes represent the isothermally buoyant simulations.
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Same as Figure 7, but for ζ = 1.
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Field lines plotted from the y = 0 plane at t = 600 t 0. The white field lines go through the core of the MFR, and the red and blue field lines are traced from regions where B  y  changes sign in the y = 0 plane. The yellow field lines are traced from the narrow band of positive B  y  below the blue/red field lines.
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Same as Figure 6, but for ζ = 2.
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Field lines at two different times late in the ζ = 0.5 simulation from above and the side. Red, pink, blue, green, and yellow field lines are traced from the bottom boundary of the simulation domain, at ﹩{s}^{2}={x}^{2}+{(y\pm {r}_{0})}^{2}﹩ for s = 3, 5.5,  7,  9.5, and  12 L 0, respectively. Orange field lines are traced from the upper photosphere. Because the field lines are line-tied at the bottom boundary, in the absence of the reconnection or diffusion, the field lines shown in the figures are the same at each time step.
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Field lines plotted from the y = 0 plane at the time when the ζ = 2 MFR is about to emerge. The white field lines go through the core of the MFR, and the black field lines are traced from regions where B  y  changes sign in the y = 0 plane.
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Same as Figure 8, but for ζ = 2.
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Same as Figure 8, but for ζ = 1.
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Same as Figure 6, but for ζ = 1.
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Same as Figure 7, but for ζ = 2.
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Height–time diagrams of the unsigned vertical magnetic flux, showing a fraction of the simulation domain in the z-direction. The horizontal dashed line is at z = 0 and the vertical solid line shows the time at which the peak photospheric field strength first exceeds 0.05B 0. The “X” shows the time and location at which the Parker instability criterion is first exceeded. Top row: ζ = 0 and ζ = 0.5. Bottom row: ζ = 1 and ζ = 2. The blue curve shows the location of the front of the magnetic flux pileup (see text).
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: (a) Flux emergence rate as a function of emerged flux for each simulation. (b) Same data, but including results from Norton et al. (2017). Orange crosses (diamonds) are observational (simulation) results reported in that paper. Black diamonds are 2D simulation results similar to the ones reported in Leake et al. (2017).
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Field lines, colored by curvature magnitude, plotted just below the photosphere right before emergence. Top row: ζ = 0 and ζ = 0.5. Bottom row: ζ = 1 and ζ = 2.
Paper: Axisymmetric Pulsar Magnetosphere Revisited
Authors: Rui Hu, Andrei M. Beloborodov
Figure caption: Top: time-averaged charge densities of electrons ρ  e , positrons ρ  p , and ions ρ  i . Bottom: contributions of the electrons, positrons, and ions to the poloidal current density. The sign of the poloidal current is set equal to the sign of J  r .
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: (a) Location and (b) rise speed of the front of the MFR as determined from Figure 20. The black horizontal lines in panel (b) show the maximum rise velocity of magnetic flux at a depth of 65 Mm and 20 Mm as inferred by Ilonidis et al. (2011; dashed line) and Birch et al. (2016; solid line), respectively. Panel (c) shows a zoomed-in version of panel (b).
Paper: Axisymmetric Pulsar Magnetosphere Revisited
Authors: Rui Hu, Andrei M. Beloborodov
Figure caption: Time-averaged  E  ·  J  (left), ( J  ×  B ) ϕ /c (middle), and the local average of energy in units of m  e  c 2 (right).
Paper: Axisymmetric Pulsar Magnetosphere Revisited
Authors: Rui Hu, Andrei M. Beloborodov
Figure caption: Time-averaged poloidal current density J pol, total charge density ρ, and toroidal magnetic field B  ϕ . Green curves show the poloidal magnetic field lines (poloidal cross sections of the axisymmetric magnetic flux surfaces), uniformly spaced in the magnetic flux function. The white dashed vertical line indicates the light cylinder. The plots have a resolution of 42 times coarser than the native resolution in the simulation.
Paper: The Emergence of Toroidal Flux Ropes with Different Twist Rising at the Same Speed
Authors: Kalman J. Knizhnik, Mark G. Linton, James E. Leake
Figure caption: Magnetic flux through the photosphere for each simulation.
Paper: Axisymmetric Pulsar Magnetosphere Revisited
Authors: Rui Hu, Andrei M. Beloborodov
Figure caption: Time-averaged electromagnetic power converted to plasma energy inside a sphere of radius r, L diss(r) = ∫ E  ·  J  dV, is shown as a function of r (blue curve). L diss(r) is normalized to the spin-down rate of the star L sd. The other three curves show the contributions to L diss from three components of the scalar product  E  ·  J  in the “magnetic flux coordinates” with basis vectors along  B  pol,  e   ϕ , and  B  pol ×  e   ϕ . The latter basis vector is perpendicular to the magnetic flux surface (parallel to ∇f).
Paper: Axisymmetric Pulsar Magnetosphere Revisited
Authors: Rui Hu, Andrei M. Beloborodov
Figure caption: Left: energy distribution of electrons (top) and positions (bottom) sampled at t = 98 R ⋆/c in the zone around the Y-point: 4.9R ⋆ < x < 5.1R ⋆ and ∣z∣ < 0.6R ⋆. Right: distribution of the same sampled particles over p  ϕ /p pol, the ratio of toroidal and poloidal components of the particle’s momentum. One can see that the vast majority of particles in the Y-point region move in the toroidal direction, ∣p  ϕ /p pol∣ ≫ 1.
Paper: Axisymmetric Pulsar Magnetosphere Revisited
Authors: Rui Hu, Andrei M. Beloborodov
Figure caption: Ratio of E ⊥/B pol, shown for a snapshot of the simulation at t = 119R ⋆/c. This figure is a zoom-in of the Y-point region and uses the full resolution of the simulation. Like other figures, green curves show poloidal magnetic field lines (axisymmetric flux surfaces) uniformly spaced in the poloidal magnetic flux function. The black dashed line is the boundary of the zone of negligible B  ϕ  (∣B  ϕ /B pol∣ < 0.1).
Paper: Axisymmetric Pulsar Magnetosphere Revisited
Authors: Rui Hu, Andrei M. Beloborodov
Figure caption: The radial flux of particle number (for each of the three species) through a cross section defined by ∣z∣ < 0.15R ⋆, as a function of x (distance from the rotation axis). The chosen cross section is sufficiently large to cover the equatorial outflow through the magnetic nozzle. Each of the three fluxes was averaged over the last revolution, 176 < ct/R ⋆ < 213, and normalized to I 0/e = μΩ2/ce.
Paper: Axisymmetric Pulsar Magnetosphere Revisited
Authors: Rui Hu, Andrei M. Beloborodov
Figure caption: Time-averaged number density of gamma rays n  γ  (left), gamma-ray emission rate per unit volume ﹩{\dot{n}}_{\mathrm{em}}﹩ (middle), and e ± creation rate ﹩{\dot{n}}_{\pm }﹩ per unit volume (right).
Paper: Axisymmetric Pulsar Magnetosphere Revisited
Authors: Rui Hu, Andrei M. Beloborodov
Figure caption: Time-averaged matter energy density U  m  (left), electromagnetic energy density U  EB  = (E 2 + B 2)/8π (middle), and their ratio (right). Note the field enhancement in the separatrix current sheet.
Paper: Axisymmetric Pulsar Magnetosphere Revisited
Authors: Rui Hu, Andrei M. Beloborodov
Figure caption: Time-averaged toroidal four-velocities u  ϕ  of the electromagnetic field ( E  ×   B  drift; left), electrons (middle), and positrons (right). The figure shows a zoom-in of the Y-point region.
Paper: Axisymmetric Pulsar Magnetosphere Revisited
Authors: Rui Hu, Andrei M. Beloborodov
Figure caption: Radial hydrodynamic speed v  r  for each species, measured at z = ±0.15R ⋆, as a function of x (distance from the rotation axis), averaged over the last revolution.
Paper: Axisymmetric Pulsar Magnetosphere Revisited
Authors: Rui Hu, Andrei M. Beloborodov
Figure caption: Average ϕ velocity of an emitted photon.
Paper: Axisymmetric Pulsar Magnetosphere Revisited
Authors: Rui Hu, Andrei M. Beloborodov
Figure caption: Plasmoids formed by magnetic reconnection in the equatorial outflow. The snapshot was taken at t = 213.2 R ⋆/c, at the end of the simulation. Top: electron density n  e . Bottom: contours of the normalized magnetic flux function ﹩f/{f}_{\max }﹩.
Paper: Axisymmetric Pulsar Magnetosphere Revisited
Authors: Rui Hu, Andrei M. Beloborodov
Figure caption: Vertical speed of the plasma flow toward the equatorial current sheet. It approximately represents the reconnection speed, which is originally defined as the drift speed ﹩{v}_{D}^{\prime} ﹩ in the wind rest frame ﹩K^{\prime} ﹩ (where the horizontal drift vanishes). Here, the hydrodynamic speed of electrons was used as a proxy of the plasma flow. It was measured at z = ±0.15R ⋆, as a function of x. The values are averaged over the last revolution, 176 < ct/R ⋆ < 213.
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: GRB 180618A light curves at the gamma-ray, X-ray, ultraviolet and optical bands. The data correspond to the Swift BAT, Swift XRT, Swift UVOT white, v, b, u, uvw1, uvm2, uvw2 bands; LT RINGO3 BV, R, I bands; and LT IO:O g, r, i bands. The Swift BAT and XRT observations were obtained from the web interface provided by the Leicester University (Evans et al. 2009); the BAT data were binned to a signal-to-noise ratio of 7, and the absorbed 0.3−10 keV XRT light curve was converted to the observed flux density at 1 keV. For completeness, we include the optical observations and upper limits reported in the Gamma-ray Coordination Network (GCN) from the MASTER II (Tyurina et al. 2018), Tien Shan Astronomical Observatory (Mazaeva et al. 2018), and Xinglong-2.16 m (Zhu et al. 2018). Note that the GCN observations do not include filter corrections. In the x-axis, T 0 corresponds to the BAT trigger time. In the y-axis, the flux density is converted to the RINGO3 R magnitude. Detections have 1σ error bars, and nondetections are presented as 3σ upper limits—note that the MASTER data have 5σ upper limits. In the bottom panel, we present the temporal evolution of the photon index in the GBM 8 keV−40 MeV gamma-ray band, the BAT 15−150 keV gamma-ray band, the XRT 0.3−10 keV X-ray band, and the RINGO3 1.2−3.5 eV optical band.
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: Observing fields of the GRB 180618A sky region. The GRB 180618A location is labeled in red, the stars (S) in light brown, and the galaxies (G) in black. (a) The 2 m LT I-band RINGO3 image of the GRB 180618A optical transient. (b) The r-band LBC image from the 8.4 m LBT. (c) The LBT z-band image. The field of view of the magnified LBT images corresponds to the white rectangle of panel (a). The LBT images reveal three galaxies at a similar redshift near the UVOT subarcsec localization of GRB 180618A (shown in red at the 90% confidence level). The G1 is the host galaxy of short GRB 180618A, with spectroscopic redshift z = 0.554 ± 0.001.
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: GRB 180618A light curves at 64 ms resolution as detected by the BAT and the GBM instruments. (a) Count rate per enabled detector of the 15−350 keV energy band of the BAT. (b) Count rates of the 8−900 keV energy band of the GBM sodium iodide (NaI) detector, and the 200 keV−40 MeV of the GBM bismuth germanate (BGO) detector. In a different y-axis, we present the evolution of the peak energy (E peak); the values were derived from a cutoff power-law model fit to the 8 keV−40 MeV ν F  ν  spectrum. In the x-axis, T 0 corresponds to the BAT trigger time.
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: High-energy properties of GRB 180618A and comparison with catalog GRBs; those with duration T 90 > 2 s are displayed in gray, and those with T 90 < 2 s in blue (Kouveliotou et al. 1993). (a) BAT-band hardness ratio and duration of GRB 180618A (t 1), the ≈0.3 s short gamma-ray pulse (t 2), and its ≈45 s extended gamma-ray emission (t 3). The background data correspond to the short hard and long soft bimodal clustering of the BAT GRB catalog (Kouveliotou et al. 1993; Lien et al. 2016). (b) Comparison of the ≈0.3 s short GRB 180618A flux F and the fluence S (marked in orange) with the GRB sample from the GBM catalog (von Kienlin et al. 2020; Poolakkil et al. 2021). Note that the GRB 180618A flux and fluence have been recalculated to match the 10−103 keV energy range of the GBM catalog. (c) Photon index β PI and peak energy E peak of GRB 180618A (marked in orange).
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: Rest-frame peak energy (E peak) and isotropic-equivalent energy (E iso) of short GRB 180618A and its extended gamma-ray emission at redshift z = 0.554. The GRB 180618A high-energy parameters are also displayed for the redshift range z = 0.01–1.5. For reference, we include those GRBs with known redshifts classified as giant flares from magnetars (GFs; Zhang et al. 2020), short GRBs (sGRBs; D’Avanzo et al. 2014; Calderone et al. 2015; Tsvetkova et al. 2017, 2021), short GRBs with extended gamma-ray emission (sGRBEEs; D’Avanzo et al. 2014), long GRBs (lGRBs; Tsvetkova et al. 2017, 2021), and X-ray flashes (XRFs; Tsvetkova et al. 2021). For the population of long GRBs, we represent the best-fitting line from Tsvetkova et al. 2021, and the corresponding 1σ, 2σ, 3σ confidence levels. We also add the GRB counterpart of gravitational wave event GW170817 (Zhang et al. 2018), and three GRBs with early afterglows interpreted as blackbody emission from either a thermalized jet or cocoon: XRF 060218 (Campana et al. 2006; Thöne et al. 2011), GRB 101225A (Thöne et al. 2011), and GRB 171205A (D’Elia et al. 2018; Izzo et al. 2019).
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: From top to bottom: two-dimensional MODS-2 spectra of the galaxy G2 and the GRB 180618A host galaxy (G1), corresponding night-sky emission lines, and one-dimensional spectrum of the G1 galaxy. In the G1 spectrum, we identify two oxygen emission lines (corresponding to [O II] and [O III]) redshifted at z = 0.554 ± 0.001. The night-sky spectrum displayed here demonstrates that both oxygen emission lines (marked in solid red arrows) are not unsubtracted night-sky emission lines; the [O II] line is not coincident with any night-sky line, and the [O III] line is found between two (dotted red lines).
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: RINGO3 BV-, R-, I-band and UVOT white-, u-band data modeled with smoothly connected broken power laws that have a common time break across bands. The results of the fit are a break at t break = 2120 ± 60 s post-burst and power-law indexes of α 1 = 0.46 ± 0.02 pre-break and α 2 = 4.6 ± 0.3 post-break with χ 2/ dof = 128/116. We also show with a dotted line the best-fitting model normalized to the near-ultraviolet UVOT uvw1 band, which has a power-law decay α  uvw1 > 1.7 pre-break. Detections have 1σ error bars, and nondetections are presented as 3σ upper limits.
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: RINGO3 photometric analysis of the field stars (S) in Figure 3 using the temporal binning of the GRB 180618A light curves. Note that stars S1 and S2 are not included in the analysis because the LT repointed to the GRB 180618A coordinates after the IO:O observations, and they fall outside of the revised RINGO3 field of view. From left to right, panels correspond to the RINGO3 BV, R, and I bands.
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: Estimation of the GRB 180618A redshift from the co-temporal GRB 180618A UVOT and RINGO3 data modeled with a dust-absorbed power law that includes the redshifted Lyman-limit break. (a) χ 2 distribution of the best-fitting redshifts for different values of the host galaxy extinction E(B − V)HG and photon index β PI. The confidence level contours at the 2σ level indicate a redshift z < 1.5 for GRB 180618A. (b) Best-fitting models for redshifts z = 0, 1, 2.
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: Temporal evolution of the effective temperatures (T eff), luminosities (L th), and photospheric radii (R ej) of the best-fitting blackbody models at the host galaxy rest frame (i.e., z = 0.554). The shaded gray area corresponds to the thermal contribution from the magnetar wind nebula, and the dotted gray line is the expected evolution of the temperature, luminosity, and radius for an optically thin regime.
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: GRB 180618A best-fitting blackbody models to joint RINGO3/UVOT data at the observer rest frame. Note that the model accounts for Galactic dust extinction but does not include the host galaxy dust contribution.
Paper: A Short Gamma-Ray Burst from a Protomagnetar Remnant
Authors: N. Jordana-Mitjans, C. G. Mundell, C. Guidorzi, R. J. Smith, E. Ramírez-Ruiz, B. D. Metzger, S. Kobayashi, A. Gomboc, I. A. Steele, M. Shrestha, M. Marongiu, A. Rossi, B. Rothberg
Figure caption: Modeling of the GRB 180618A RINGO3 optical emission with power-law models. Note that the model accounts for Galactic dust extinction but does not include the host galaxy dust contribution.