adsabs/AstroCLIMB huggingface dataset:
Paper: Trans-Neptunian Object Colors as Evidence for a Past Close Stellar Flyby to the Solar System
Authors: Susanne Pfalzner, Frank W. Wagner, Paul Gibbon
Figure caption: Entire parameter space and 100 au sized disk. Scatter plot of the TNOs’ inclinations as a function of perihelion distance for (a) the entire parameter space and (c) a 100 au sized disk. Scatter plot of the TNOs’ eccentricities as a function of perihelion distance for (b) the entire parameter space and (d) a 100 au sized disk.
Paper: Trans-Neptunian Object Colors as Evidence for a Past Close Stellar Flyby to the Solar System
Authors: Susanne Pfalzner, Frank W. Wagner, Paul Gibbon
Figure caption: Connection between TNO color and eccentricity. The left column illustrates the observational data of M. Ali-Dib et al. (2021) and M. Marsset et al. (2019), and the right column shows the numerical results from our flyby simulation. Panels (a) and (b) display scatter plots of the TNOs’ eccentricity as a function of periastron distance. Panels (c) and (d) show the corresponding color distributions distinguishing between objects with e > 0.42 and e < 0.42. The colors in panels (b) and (d) are as defined in Figure 1(a). For the data of M. Marsset et al. (2019) we excluded the centaurs.
Paper: Trans-Neptunian Object Colors as Evidence for a Past Close Stellar Flyby to the Solar System
Authors: Susanne Pfalzner, Frank W. Wagner, Paul Gibbon
Figure caption: Other correlations between colors and dynamical parameters. Panel (a) illustrates the scarcity of very red objects among the detached TNOs in the observations (top) and simulations (bottom). Panel (b) depicts the inclination as a function of the initial distance of the TNOs.
Paper: Trans-Neptunian Object Colors as Evidence for a Past Close Stellar Flyby to the Solar System
Authors: Susanne Pfalzner, Frank W. Wagner, Paul Gibbon
Figure caption: Surface density dependence. Origin of the high- and low-inclination TNOs as in Figure 2(d). However, here we show a comparison of the test particle distribution (black), with those assuming a 1/r (blue) and a 1/r3/2 (red) surface distribution in the preflyby disk.
Paper: Trans-Neptunian Object Colors as Evidence for a Past Close Stellar Flyby to the Solar System
Authors: Susanne Pfalzner, Frank W. Wagner, Paul Gibbon
Figure caption: Predictions for LSST. Panels (a) and (b) for TNOs with perihelion distances exceeding 60 au. Panel (c) shows the colors of highly inclined and retrograde objects with p < 100 au. Panel (d) illustrates the corresponding color distributions.
Paper: Trans-Neptunian Object Colors as Evidence for a Past Close Stellar Flyby to the Solar System
Authors: Susanne Pfalzner, Frank W. Wagner, Paul Gibbon
Figure caption: Long-term evolution. Connection between TNOs’ colors, inclinations (a), and eccentricities (b) after 1 Gyr. Panels (c) and (d) depict the corresponding color distributions.
Paper: Trans-Neptunian Object Colors as Evidence for a Past Close Stellar Flyby to the Solar System
Authors: Susanne Pfalzner, Frank W. Wagner, Paul Gibbon
Figure caption: Injected TNOs. Origin distribution of TNOs injected within 29 au, which may have been partly captured as irregular moons.
Paper: Energy Cascade and Damping in Fast-mode Compressible Turbulence
Authors: Chuanpeng Hou, Huirong Yan, Siqi Zhao, Parth Pavaskar
Figure caption: Angle-dependent collisionless damping in the near-isotropic cascade of fast-mode turbulence. (a) PSD distribution in k⊥–k∥ space calculated from the 3D hybrid simulation. (b) PSD distribution in k⊥–k∥ space calculated from the 2D PIC simulation. (c) PSD distribution in k⊥–k∥ space calculated from the 2D PIC simulation with a higher resolution. (d) Theoretical PSD distribution in k⊥–k∥ space according to Equation (5).
Paper: Energy Cascade and Damping in Fast-mode Compressible Turbulence
Authors: Chuanpeng Hou, Huirong Yan, Siqi Zhao, Parth Pavaskar
Figure caption: The 1D energy spectrum of compressible turbulence. (a) Integrated 1D-PSD of the fast-mode velocity field as a function of kdi obtained from the 3D hybrid simulation. (b) Integrated 1D-PSD of the fast-mode velocity field as a function of kdi obtained from the 2D PIC simulation. (c) Integrated 1D-PSD of the fast-mode velocity field as a function of kdi obtained from the high-resolution 2D PIC simulation. (d) Filtered SF2,v of velocity field from the 3D hybrid simulation, as defined by Equation (2). (e) SF2,v of velocity field from the 2D PIC simulation. (f) SF2,v of velocity field from the high-resolution 2D PIC simulation. In all panels, the fitted scalings are shown as dashed lines.
Paper: Energy Cascade and Damping in Fast-mode Compressible Turbulence
Authors: Chuanpeng Hou, Huirong Yan, Siqi Zhao, Parth Pavaskar
Figure caption: Energy source for particle heating. (a) Temporal evolution of proton and electron temperatures from PIC simulation. The dashed line marks the time corresponding to panel (b). (b) Probability density function of the temperature ratio between intermittent and nonintermittent regions. The mean temperature ratio is shown by dashed lines. (c) Proton temperature in the perpendicular magnetic field (x–y) plane, sliced at z = 0 di from 3D hybrid simulation. (d) Same as (c) but for the divergence of the velocity field.
Paper: Energy Cascade and Damping in Fast-mode Compressible Turbulence
Authors: Chuanpeng Hou, Huirong Yan, Siqi Zhao, Parth Pavaskar
Figure caption: Spatial distribution of near-isotropic features in the compressible turbulence. (a) Isosurfaces of the velocity component vy from the 3D hybrid simulation, plotted at levels −0.2vA and 0.2vA. The color bar indicates the range of vy values across three orthogonal slices. (b) Distribution of proton vy in the 2D PIC simulation. The direction of the background magnetic field is shown by black arrows.
Paper: The Type II SN 2025pht in NGC 1637: A Red Supergiant with Carbon-rich Circumstellar Dust as the First JWST Detection of a Supernova Progenitor Star
Authors: Charles D. Kilpatrick, Aswin Suresh, Kyle W. Davis, Maria R. Drout, Ryan J. Foley, Alexander Gagliano, Wynn V. Jacobson-Galán, Ravjit Kaur, Kirsty Taggart, Jason Vazquez
Figure caption: Top: our Keck/LRIS spectrum of SN 2025pht (black) obtained on 2025 July 27 as described in Section 2.2 and compared with a spectrum of SN 2004et (gray) that is most consistent with our observation (Section 3.1). We identify key features that aid in our classification of SN 2025pht as a typical SN II, likely in its plateau phase during this epoch and with an Hα velocity derived from the trough of its blueshifted absorption of 6800 ± 100 km s−1. Bottom: a continuum-normalized section of the SN 2025pht spectrum centered on the rest wavelength of Na I D at the redshift of NGC 1637 (≈5906 Å). While we detect the Milky Way components of Na I D, we do not detect any Na I D absorption from NGC 1637, leading us to conclude that there is an insignificant magnitude of line-of-sight extinction to SN 2025pht in this galaxy. All spectra are available via WISeREP (O. Yaron & A. Gal-Yam 2012).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Type II SN 2025pht in NGC 1637: A Red Supergiant with Carbon-rich Circumstellar Dust as the First JWST Detection of a Supernova Progenitor Star
Authors: Charles D. Kilpatrick, Aswin Suresh, Kyle W. Davis, Maria R. Drout, Ryan J. Foley, Alexander Gagliano, Wynn V. Jacobson-Galán, Ravjit Kaur, Kirsty Taggart, Jason Vazquez
Figure caption: Left: a color image of NGC 1637 constructed from F150W (blue), F277W (green), and F444W (red) images obtained with JWST/NIRCam on 2024 October 8 showing a 1.0 × 0.9 arcmin2 portion of the galaxy. We highlight a 2.7 × 2.4 arcsec2 region centered on the site of SN 2025pht with a white box toward the bottom of the frame. Right: a series of grayscale frames showing HST/WFC3 F336W imaging of SN 2025pht obtained on 2025 July 31, with the centroid of the SN marked in red. We show the same region obtained by HST/WFC3 in F336W, F555W, and F814W obtained on 2024 August 3; by JWST/NIRCam in F150W, F277W, and F444W on 2024 October 8; and by JWST/MIRI on 2024 February 5. We show the location of the SN with the same red circle, demonstrating that there is a credible counterpart detected in all of the JWST images as discussed in Section 4.1.
Paper: The Type II SN 2025pht in NGC 1637: A Red Supergiant with Carbon-rich Circumstellar Dust as the First JWST Detection of a Supernova Progenitor Star
Authors: Charles D. Kilpatrick, Aswin Suresh, Kyle W. Davis, Maria R. Drout, Ryan J. Foley, Alexander Gagliano, Wynn V. Jacobson-Galán, Ravjit Kaur, Kirsty Taggart, Jason Vazquez
Figure caption: Top: same as Figure 4, but for graphitic and silicate dust models fit only to the JWST/NIRCam photometry. This model results in similar posteriors to the full SED fit. Middle: same as the top panel, but using only JWST/NIRCam and MIRI photometry from 2024 February 5 to minimize the effects of variability. The posteriors for the silicate model still overpredict the F770W flux. Bottom: same as Figure 4, but setting the dust shell boundaries using Rout/Rin = 10 in our model as described in Section 4.3.2. The silicate model again overpredicts the F770W flux.
Paper: The Type II SN 2025pht in NGC 1637: A Red Supergiant with Carbon-rich Circumstellar Dust as the First JWST Detection of a Supernova Progenitor Star
Authors: Charles D. Kilpatrick, Aswin Suresh, Kyle W. Davis, Maria R. Drout, Ryan J. Foley, Alexander Gagliano, Wynn V. Jacobson-Galán, Ravjit Kaur, Kirsty Taggart, Jason Vazquez
Figure caption: The probability density for the bolometric correction to ≈8000 Å (i.e., for F814W, Ic, Ij, and i bands) for 20 pre-SN counterparts to SNe II from S. Healy et al. (2024; blue; see their Table A.2) compared with the bolometric correction derived for WFC3/UVIS F814W in our modeling of SN 2017eaw, SN 2023ixf, SN 2024ggi, and SN 2025pht (red; see Section 5.2). As the latter events have well-sampled SEDs, including at >2 μm with Spitzer and JWST, we consider their optical bolometric corrections, where most SN II counterparts are detected to be more reliable than for SN II counterparts that lack IR photometry. We measure the average and standard deviation of both distributions as 0.20 ± 0.23 mag and −2.58 ± 1.24 mag.
Paper: The Type II SN 2025pht in NGC 1637: A Red Supergiant with Carbon-rich Circumstellar Dust as the First JWST Detection of a Supernova Progenitor Star
Authors: Charles D. Kilpatrick, Aswin Suresh, Kyle W. Davis, Maria R. Drout, Ryan J. Foley, Alexander Gagliano, Wynn V. Jacobson-Galán, Ravjit Kaur, Kirsty Taggart, Jason Vazquez
Figure caption: Our best-fitting SEDs to the 2024 detections of the SN 2025pht counterpart as discussed in Section 4.3. All SEDs correspond to a source with ﹩{\mathrm{log}}\,(L/{L}_{\odot })\approx 5.0﹩. Motivated by the cool blackbody fit, we attempt fits to MARCS SEDs of RSGs reddened via dust prescriptions using dusty as described in Section 4.3.2. While a purely graphitic dust prescription captures the overall shape of the SED out to 8 μm, the silicate model overpredicts this measurement, leading us to conclude that the SN 2025pht counterpart is consistent with a graphitic dust model.
Paper: The Type II SN 2025pht in NGC 1637: A Red Supergiant with Carbon-rich Circumstellar Dust as the First JWST Detection of a Supernova Progenitor Star
Authors: Charles D. Kilpatrick, Aswin Suresh, Kyle W. Davis, Maria R. Drout, Ryan J. Foley, Alexander Gagliano, Wynn V. Jacobson-Galán, Ravjit Kaur, Kirsty Taggart, Jason Vazquez
Figure caption: A series of HST/WFPC2 (top) and WFC3 (bottom) images in F814W and F336W showing the detection of SN 2025pht (bottom right) and the detection of its counterpart from 2001 and eventual disappearance in 2024, demonstrating that the pre-explosion counterpart had some long time baseline variability over this 23 yr span. We discuss the significance of this measurement in Section 4.2.
Paper: The First Radio-bright Off-nuclear Tidal Disruption Event AT 2024tvd Reveals the Fastest-evolving Double-peaked Radio Emission
Authors: Itai Sfaradi, Raffaella Margutti, Ryan Chornock, Kate D. Alexander, Brian D. Metzger, Paz Beniamini, Rodolfo Barniol Duran, Yuhan Yao, Assaf Horesh, Wael Farah, Edo Berger, Nayana A. J., Yvette Cendes, Tarraneh Eftekhari, Rob Fender, Noah Franz, Dave A. Green, Erica Hammerstein, Wenbin Lu, Eli Wiston, Yirmi Bernstein, Joe Bright, Collin T. Christy, Luigi F. Cruz, David R. DeBoer, Walter W. Golay, Adelle J. Goodwin, Mark Gurwell, Garrett K. Keating, Tanmoy Laskar, James C. A. Miller-Jones, Alexander W. Pollak, Ramprasad Rao, Andrew Siemion, Sofia Z. Sheikh, Nadav Shoval, Sjoert van Velzen
Figure caption: Radio luminosity evolution of a selection of known TDEs (ASASSN-14li, K. D. Alexander et al. 2016; ASASSN-15oi, A. Horesh et al. 2021a; AT 2019dsg, R. Stein et al. 2021; AT 2018hyz, Y. Cendes et al. 2022; AT 2019azh, A. J. Goodwin et al. 2022; I. Sfaradi et al. 2022; AT 2020vwl, A. J. Goodwin et al. 2023) and AT 2024tvd (this work; 10 GHz marked with red stars; 15.5 GHz marked with orange stars). Observations of the same TDE are connected with lines, and 3σ upper limits are plotted with triangles. The radio emission from the off-nuclear TDE AT 2024tvd reveals an extremely fast evolution compared to other TDEs, with a fast rise between Δt = 88 and 131 days, followed by a fast decline up to Δt = 173 days. Then, at Δt = 194 days, and about ∼20 days since the last observation of the first radio flare, a second fast-rising radio flare emerges.
Paper: The First Radio-bright Off-nuclear Tidal Disruption Event AT 2024tvd Reveals the Fastest-evolving Double-peaked Radio Emission
Authors: Itai Sfaradi, Raffaella Margutti, Ryan Chornock, Kate D. Alexander, Brian D. Metzger, Paz Beniamini, Rodolfo Barniol Duran, Yuhan Yao, Assaf Horesh, Wael Farah, Edo Berger, Nayana A. J., Yvette Cendes, Tarraneh Eftekhari, Rob Fender, Noah Franz, Dave A. Green, Erica Hammerstein, Wenbin Lu, Eli Wiston, Yirmi Bernstein, Joe Bright, Collin T. Christy, Luigi F. Cruz, David R. DeBoer, Walter W. Golay, Adelle J. Goodwin, Mark Gurwell, Garrett K. Keating, Tanmoy Laskar, James C. A. Miller-Jones, Alexander W. Pollak, Ramprasad Rao, Andrew Siemion, Sofia Z. Sheikh, Nadav Shoval, Sjoert van Velzen
Figure caption: Broadband radio SEDs of the off-nuclear TDE AT 2024tvd. The left panel shows the radio SEDs of the first radio flare, and the right panel is for the second radio flare. Detections obtained with different radio telescopes are marked with different markers (circles for the VLA, diamonds for ALMA, squares for AMI-LA, and pentagons for the ATA), and triangles mark 3σ upper limits. We fitted these SEDs with the broken power-law function described in Equation (4) (see detailed discussion in Section 4.1).
Paper: The First Radio-bright Off-nuclear Tidal Disruption Event AT 2024tvd Reveals the Fastest-evolving Double-peaked Radio Emission
Authors: Itai Sfaradi, Raffaella Margutti, Ryan Chornock, Kate D. Alexander, Brian D. Metzger, Paz Beniamini, Rodolfo Barniol Duran, Yuhan Yao, Assaf Horesh, Wael Farah, Edo Berger, Nayana A. J., Yvette Cendes, Tarraneh Eftekhari, Rob Fender, Noah Franz, Dave A. Green, Erica Hammerstein, Wenbin Lu, Eli Wiston, Yirmi Bernstein, Joe Bright, Collin T. Christy, Luigi F. Cruz, David R. DeBoer, Walter W. Golay, Adelle J. Goodwin, Mark Gurwell, Garrett K. Keating, Tanmoy Laskar, James C. A. Miller-Jones, Alexander W. Pollak, Ramprasad Rao, Andrew Siemion, Sofia Z. Sheikh, Nadav Shoval, Sjoert van Velzen
Figure caption: Radio images of the field of AT 2024tvd. Left panel: the first VLA observation in X band at Δt = 88 days, resulting in a null detection of the TDE and a detection of the nucleus of the host. Right panel: the VLA C-band image at Δt = 160 days, showing both the emission from the TDE and the emission from the host galaxy. The positions of the TDE and the nucleus obtained from the HST image (Y. Yao et al. 2025b) are marked with a cross and a plus sign, respectively. The size of the VLA clean beams is shown with a yellow ellipse in the lower left corner of each VLA image. The VLA images are scaled differently in order to show the full range of flux densities from the TDE and from the host galaxy nucleus.
Paper: The First Radio-bright Off-nuclear Tidal Disruption Event AT 2024tvd Reveals the Fastest-evolving Double-peaked Radio Emission
Authors: Itai Sfaradi, Raffaella Margutti, Ryan Chornock, Kate D. Alexander, Brian D. Metzger, Paz Beniamini, Rodolfo Barniol Duran, Yuhan Yao, Assaf Horesh, Wael Farah, Edo Berger, Nayana A. J., Yvette Cendes, Tarraneh Eftekhari, Rob Fender, Noah Franz, Dave A. Green, Erica Hammerstein, Wenbin Lu, Eli Wiston, Yirmi Bernstein, Joe Bright, Collin T. Christy, Luigi F. Cruz, David R. DeBoer, Walter W. Golay, Adelle J. Goodwin, Mark Gurwell, Garrett K. Keating, Tanmoy Laskar, James C. A. Miller-Jones, Alexander W. Pollak, Ramprasad Rao, Andrew Siemion, Sofia Z. Sheikh, Nadav Shoval, Sjoert van Velzen
Figure caption: Radio light curves of the off-nuclear TDE AT 2024tvd at different frequencies. We plot temporal power laws for different segments of these light curves (with the reference initial time being the optical discovery), showing the fast rise and decay in both flares.
Paper: Precision Measurement of Large Shear Signals
Authors: Jiarui Sun, Jun Zhang, Li Cui, Alessandro Sonnenfeld, Xin Wang
Figure caption: An example of the shear errors using irregular galaxies with SNR = 10. The color scheme and line styles are the same as those in Figure 2.
Paper: Absence of Radio Emission Reveals an Exceptionally Weak Explosion of the Putative Historical Supernova Pa 30
Authors: Yi-Xuan Shao, Ping Zhou, Xiao Zhang, Zhi-Yu Zhang, Yang Chen, Qin Han, Di Li, Xiang-Dong Li, Jian-Bin Weng, Yong Shao
Figure caption: Left: The 1 GHz radio surface brightness vs. angular area diagram of shell-type SNRs, using the catalog by D. A. Green (2025). The diamond markers represent historical SNRs. The “+” markers show two newly found SNRs, G181.1+9.5 (R. Kothes et al. 2017) and G116.6-26.1 (E. M. Churazov et al. 2022) with low radio surface brightness. Right: The Σ–D diagram, with the gray dots representing the shell-type SNRs with known distance taken from M. Z. Pavlović et al. (2013) and the diamond markers showing young SNRs with good distance measurements. The dashed lines show three exemplified cases with different SN kinetic energy (ESN), ejecta mass (Mej), and ambient density (n0), where s = 2.3 and ϵB = 0.001 are assumed. The blue shaded region shows the area predicted for most SNRs with s = 2–2.5, ESN = 1050–2 × 1051 erg, Mej = 1–4 M⊙, n0 = 0.05–1 cm−3, and ϵB = 0.001–0.1. The red triangle denotes the 3σ upper limit of Pa 30, extrapolated from 6 GHz using a frequency spectral index of 0.65.
Paper: Absence of Radio Emission Reveals an Exceptionally Weak Explosion of the Putative Historical Supernova Pa 30
Authors: Yi-Xuan Shao, Ping Zhou, Xiao Zhang, Zhi-Yu Zhang, Yang Chen, Qin Han, Di Li, Xiang-Dong Li, Jian-Bin Weng, Yong Shao
Figure caption: Synchrotron spectra predicted by the model of (T. Ko et al. 2024b) with electron energy spectral index s = 2.5 and s = 3. The orange and blue lines represent the outer region (SNR shock) and inner region (termination shock), respectively. The solid, dashed–dotted, and dotted refer to different electron acceleration efficiencies (corresponding to optimistic, fiducial, and pessimistic assumptions, respectively): ϵe = 2 × 10−3, 5 × 10−4, and 2 × 10−4 for s = 2.5 and ϵe = 5 × 10−2, 1 × 10−2, and 5 × 10−3 for s = 3, respectively. The red and green arrows show the upper limit of the Pa 30 field and the central source J005311 in this work.
Paper: Absence of Radio Emission Reveals an Exceptionally Weak Explosion of the Putative Historical Supernova Pa 30
Authors: Yi-Xuan Shao, Ping Zhou, Xiao Zhang, Zhi-Yu Zhang, Yang Chen, Qin Han, Di Li, Xiang-Dong Li, Jian-Bin Weng, Yong Shao
Figure caption: Upper left: WISE image of the Pa 30 field; red and green show 22 μm under two intensity scales, and blue shows 12 μm. Upper right: XMM-Newton X-ray flux image in 0.3–2 keV. Lower left: VLA 1.5 GHz (L band) image. Lower right: VLA 6.0 GHz (C band) image. The white circles are 114﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 in radius centered on the central star J005311 (﹩{\rm{R}}.{\rm{A}}.\,=\,0{0}^{{\rm{h}}}5{3}^{{\rm{m}}}11\mathop{.}\limits^{{\rm{s}}}2,{\rm{decl}}.\,=\,+{67}^{\circ }3{0}^{{\rm{{\prime} }}}2\mathop{.}\limits^{\unicode{x02033}}4﹩; R. A. Fesen et al. 2023). The cyan “x” markers represent the location of the compact sources. The green ellipse in the lower-left corner of both VLA images represents the synthesized beam. The color bars show the flux density in units of Jy/beam.
Paper: The Impact of Alfvénic Shear Flow on Magnetic Reconnection and Turbulence
Authors: Tamar Ervin, Alfred Mallet, Stefan Eriksson, M. Swisdak, James Juno, Orlando M. Romeo, Tai Phan, Trevor A. Bowen, Roberto Livi, Phyllis L. Whittlesey, Davin E. Larson, Stuart D. Bale
Figure caption: Overview of the fields and plasma parameters used in this study for the time period surrounding a reconnection event identified by S. Eriksson et al. (2024; highlighted in purple). Panel (a) shows the trace magnetic field spectrum and associated fit for the time period associated with the reconnection event (highlighted in panels (b–d)). The right-side panels show the (b) SPANi proton velocity, (c) FIELDS fluxgate magnetometer magnetic field measurements, and (d) ion and electron temperatures measured by the SPANi and SPANe instruments. vR,T,N and BR,T,N are the radial, tangential, and normal components of the proton velocity (b) and magnetic field (c), respectively, where R is the direction from the Sun to the spacecraft, T is the cross product of the Sun’s rotation vector with R, and N = R × T (M. A. Hapgood 1992). All data have been filtered to remove time periods where the bulk of the distribution moves out of the SPANi FOV.
Paper: The Impact of Alfvénic Shear Flow on Magnetic Reconnection and Turbulence
Authors: Tamar Ervin, Alfred Mallet, Stefan Eriksson, M. Swisdak, James Juno, Orlando M. Romeo, Tai Phan, Trevor A. Bowen, Roberto Livi, Phyllis L. Whittlesey, Davin E. Larson, Stuart D. Bale
Figure caption: Comparison of (a) γtr/γ0tr, (b) τ, and (c) ﹩\sqrt{{r}_{{\rm{A}}}}=\alpha =\langle \delta u\rangle /\langle \delta b\rangle ﹩ for time periods associated with reconnection (black) vs. nonreconnection (pink) times. Reconnection periods are those identified by S. Eriksson et al. (2024).
Paper: The Impact of Alfvénic Shear Flow on Magnetic Reconnection and Turbulence
Authors: Tamar Ervin, Alfred Mallet, Stefan Eriksson, M. Swisdak, James Juno, Orlando M. Romeo, Tai Phan, Trevor A. Bowen, Roberto Livi, Phyllis L. Whittlesey, Davin E. Larson, Stuart D. Bale
Figure caption: Comparison of γtr/γ0tr (blue) and normalized flow shear (black) for (a) fast wind streams, (b) slow Alfvénic wind streams, and (c) slow wind streams. Wind is identified as fast, slow Alfvénic, or slow non-Alfvénic based on the categorization scheme of T. Ervin et al. (2024a).
Paper: The Impact of Alfvénic Shear Flow on Magnetic Reconnection and Turbulence
Authors: Tamar Ervin, Alfred Mallet, Stefan Eriksson, M. Swisdak, James Juno, Orlando M. Romeo, Tai Phan, Trevor A. Bowen, Roberto Livi, Phyllis L. Whittlesey, Davin E. Larson, Stuart D. Bale
Figure caption: Comparison of magnetic field spectral index for reconnecting periods (black) identified by S. Eriksson et al. (2024) and ambient wind (green). Panel (a) shows the spectral index associated with the trace spectra (αB) and panel (b) is the spectral index for the spectra of ∣B∣ (α∣B∣). The legend reports the mean and standard deviation of spectral indices.
Paper: The Impact of Alfvénic Shear Flow on Magnetic Reconnection and Turbulence
Authors: Tamar Ervin, Alfred Mallet, Stefan Eriksson, M. Swisdak, James Juno, Orlando M. Romeo, Tai Phan, Trevor A. Bowen, Roberto Livi, Phyllis L. Whittlesey, Davin E. Larson, Stuart D. Bale
Figure caption: Comparison of (a) vR, (b) σC, and (c) τ for time periods associated with reconnection (black) and ±10 minute near-reconnecting current sheet wind surrounding these events (purple).