adsabs/AstroCLIMB huggingface dataset:
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: Optical spectra of AT2021utq. The late-time DBSP spectrum shows host galaxy absorption lines (Na I, Ca II, Balmer series) at z = 0.127. At this redshift, the early time spectrum reported by Burke et al. (2021) exihibits a broad emission line around Hα, making it consistent with the TDE-H spectral class.
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: Histograms of the photometric TDE candidates that passed the filtering step (6) (see Table 1), color-coded by their spectroscopic classifications. For ZTF-I candidates, the spectroscopic classification is ∼93% complete at m peak < 18.75. For ZTF-II candidates, the spectroscopic classification is ∼89% complete at m  g,peak < 19.1.
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: Optical spectra of AT2021qth, compared with the SDSS spectrum of the prototype extreme coronal line emitter SDSS J0952+2143 (Komossa et al. 2008; Palaversa et al. 2016).
Paper: Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function
Authors: Yuhan Yao, Vikram Ravi, Suvi Gezari, Sjoert van Velzen, Wenbin Lu, Steve Schulze, Jean J. Somalwar, S. R. Kulkarni, Erica Hammerstein, Matt Nicholl, Matthew J. Graham, Daniel A. Perley, S. Bradley Cenko, Robert Stein, Angelo Ricarte, Urmila Chadayammuri, Eliot Quataert, Eric C. Bellm, Joshua S. Bloom, Richard Dekany, Andrew J. Drake, Steven L. Groom, Ashish A. Mahabal, Thomas A. Prince, Reed Riddle, Ben Rusholme, Yashvi Sharma, Jesper Sollerman, Lin Yan
Figure caption: Optical spectra of two TDEs that belong to the TDE-featureless subclass. We highlight the fact that the rest-frame Hα region is covered by our spectra, and no discernible emission lines are present throughout the spectral evolution.
Paper: A Metallicity Dependence on the Occurrence of Core-collapse Supernovae
Authors: Thallis Pessi, Joseph P. Anderson, Joseph D. Lyman, Jose L. Prieto, Lluís Galbany, Christopher S. Kochanek, Sebastian F. Sánchez, Hanindyo Kuncarayakti
Figure caption: The occurrence of CCSNe per unit of SF as a function of [O/H]. This is estimated by dividing the number of CCSNe, ﹩{N}_{[{\rm{O}}/{\rm{H}}],\mathrm{CCSN}}﹩, by the total SFR, SFRtot,[O/H],i , over binned intervals in the abundance axis. The violin plots show 500 bootstrap resamplings in each abundance interval of 0.2 dex. The black dots show the median of these realizations, while the dashed and solid lines show, respectively, the 1σ and the extrema of the realizations. We fit a second-order polynomial to the median values, weighting it by the 1σ uncertainties. A horizontal dashed line is shown at R [O/H],i  = 1. The orange dot shows the abundance for the Sun (Asplund et al. 2021) and the purple and blue dots show the median abundances for, respectively, the small magellanic cloud (SMC) and large magellanic cloud (LMC) (Toribio San Cipriano et al. 2017).
Paper: A Metallicity Dependence on the Occurrence of Core-collapse Supernovae
Authors: Thallis Pessi, Joseph P. Anderson, Joseph D. Lyman, Jose L. Prieto, Lluís Galbany, Christopher S. Kochanek, Sebastian F. Sánchez, Hanindyo Kuncarayakti
Figure caption: Cumulative distributions of the fraction of SF as a function of [O/H] for H II regions within individual galaxies. Each gray line is the distribution for one galaxy and the small symbols are the SF fraction rank and [O/H] of the CCSN environments within their host galaxy SF distributions. The median rank is given by the big markers, with uncertainties estimated by the median of the 1σ of 500 bootstrap resamplings of each distribution. The blue triangles and orange squares represent the galaxies in which the H II region with the highest [O/H] has a value lower or higher than ﹩12+{\mathrm{log}}_{10}({\rm{O}}/{\rm{H}})=8.6﹩ dex (indicated by the dashed line), respectively. The red circle shows the median values for the full sample.
Paper: A Metallicity Dependence on the Occurrence of Core-collapse Supernovae
Authors: Thallis Pessi, Joseph P. Anderson, Joseph D. Lyman, Jose L. Prieto, Lluís Galbany, Christopher S. Kochanek, Sebastian F. Sánchez, Hanindyo Kuncarayakti
Figure caption: The oxygen abundance NCR for the CCSNe. The red line shows the distribution for the full sample, and the blue and orange lines show, respectively, the galaxies where the largest metallicity value of their H II regions is lower or higher than ﹩12+{\mathrm{log}}_{10}({\rm{O}}/{\rm{H}})=8.6﹩ dex. An unbiased distribution with respect to metallicity should follow the dashed diagonal line in the plot. The solid lines show the median of 500 bootstrap resamplings of each cumulative distribution and the dashed lines show the 1σ of the realizations.
Paper: A Metallicity Dependence on the Occurrence of Core-collapse Supernovae
Authors: Thallis Pessi, Joseph P. Anderson, Joseph D. Lyman, Jose L. Prieto, Lluís Galbany, Christopher S. Kochanek, Sebastian F. Sánchez, Hanindyo Kuncarayakti
Figure caption: The occurrence rate of CCSNe per unit of SF as a function of [O/H], given by the O3N2 (left panel) and N2 (right panel) indicators. The violin plots show 500 bootstrap resamplings in abundance intervals of 0.06 dex. The black dots show the median of these realizations, and the dashed and solid lines show, respectively, the 1σ and the extrema of the realizations. A second-order polynomial is fit to the median values of each indicator, weighting it by the 1σ uncertainties.
Paper: Tidally Excited Inertial Waves in Stars and Planets: Exploring the Frequency-dependent and Averaged Dissipation with Nonlinear Simulations
Authors: Aurélie Astoul, Adrian J. Barker
Figure caption: Tidal dissipation from simulations as a function of frequency in the fluid frame ω/Ω*. We show the rescaled imaginary part of the Love number ﹩{\epsilon }_{{\rm{t}}}^{-2}| \mathrm{Im}\left[{k}_{2}^{2}(\omega )\right]| ﹩ (left y-axis) and the tidal quality factor ﹩{\epsilon }_{{\rm{t}}}^{2}{Q}_{\omega }^{{\prime} }﹩ (right y-axis). Colors represent energy in the differential rotation E  dr . The black solid and dashed lines show the frequency-dependent and frequency-averaged linear predictions given by Equations (7) and (10), respectively, while the purple dashed line is the frequency-averaged nonlinear tidal dissipation from Equation (9). Top: radial aspect ratio α = 0.3 and tidal forcing amplitude C t = 5 · 10−2. E  dr  is maximal when ω = −1.24 with E  dr  ≈ 6.2 · 10−4, and minimal when ω = 0.12 with E  dr  ≈ 4.6 · 10−10. Bottom: the same for a thicker envelope with α = 0.5. E  dr  is maximal when ω = −1.16 with E  dr  = 9.5 · 10−3, and minimal when ω = 2.0 with E  dr  = 1.7 · 10−8.
Paper: Tidally Excited Inertial Waves in Stars and Planets: Exploring the Frequency-dependent and Averaged Dissipation with Nonlinear Simulations
Authors: Aurélie Astoul, Adrian J. Barker
Figure caption: The same as Figure 1 but for a solar-like convective envelope with α = 0.7. (a) C t = 10−2. Differential rotation is maximal when ω = −0.22 with E  dr  = 1.6 · 10−3, and minimal when ω = 0.24 with E  dr  = 7.0 · 10−11. (b) C t = 5 · 10−2 and E = 5 · 10−5. Differential rotation is maximal when ω = −1.06 with E  dr  = 1.2 · 10−2, and minimal when ω = 0.26 with E  dr  = 2.8 · 10−8. (c) C t = 5 · 10−2 (and E = 10−5 again). E  dr  is maximal when ω = −1.14 with E  dr  = 3.1 · 10−2, and minimal when ω = 0.24 with E  dr  = 4.1 · 10−8. D  ν  can differ by up to 3 orders of magnitude at a given frequency depending on E  dr . (d) The same as (c) but colored curves instead show the evolution of D  ν  and ω/Ω* during each simulation until (in most cases) an averaged steady state is reached. Error bars indicate variations in the last 2000Ω−1 compared to the final value (purple dots).
Paper: Tidally Excited Inertial Waves in Stars and Planets: Exploring the Frequency-dependent and Averaged Dissipation with Nonlinear Simulations
Authors: Aurélie Astoul, Adrian J. Barker
Figure caption: Meridional slice of radial velocity u  r  in one quadrant with ω = −0.25 and α = 0.7 (and E = 10−5). Left: C t = 10−3 (approximately linear). Linear calculations with the spectral code Linear Solver Builder (LSB; Valdettaro et al. 2007) are indistinguishable since nonlinearities are negligible in this case. Middle: C t = 10−2. Right: C t = 5 · 10−2. Note the paradoxical decrease in u  r  when increasing C t.
Paper: Signatures of the Self-organized Criticality Phenomenon in Precursors of Gamma-Ray Bursts
Authors: Xiu-Juan Li, Yu-Peng Yang
Figure caption: The CDFs of the size differences of precursors. Panels (a)–(d) show the size difference distributions of peak fluxes (P), durations (D), rise times (t  r ), and decay times (t  d ) for n = 1 (red), n = 5 (green), n = 10 (blue), n = 20 (orange), and n = 30 (purple), respectively. The shadow regions represent the 95% confidence level, the smooth lines are the best fits. Panel (e) shows the best-fit values of q in the q-Gaussian distributions as a function of n for the precursors (the open symbols) and the main bursts (the filled symbols).
Paper: Signatures of the Self-organized Criticality Phenomenon in Precursors of Gamma-Ray Bursts
Authors: Xiu-Juan Li, Yu-Peng Yang
Figure caption: The distributions of two kinds of waiting times between precursors and main bursts (upper panel: differential and cumulative size distributions, lower panel: size difference distributions). Panels (a2) and (b2) show the size difference distributions of peak-time intervals (Δt p1) and quiescent times (Δt p2) for n = 1 (red), n = 5 (green), n = 10 (blue), n = 15 (orange), and n = 20 (purple), respectively. The shadow regions represent the 95% confidence level, the smooth lines are the best fits. Panel (e) shows the best-fit values of q in the q-Gaussian distributions as a function of n for peak-time intervals (the filled symbols) and quiescent times (the open symbols).
Paper: Signatures of the Self-organized Criticality Phenomenon in Precursors of Gamma-Ray Bursts
Authors: Xiu-Juan Li, Yu-Peng Yang
Figure caption: The size distributions of precursors (upper panel: differential distributions, lower panel: cumulative distributions). Panels (a)–(d) display the size distributions of peak fluxes (P), durations (D), rise times (t  r ), and decay times (t  d ), respectively. The green solid line is the best fit and the gray region represents the 95% confidence level, and the dotted line is marked as the threshold x 0.
Paper: Signatures of the Self-organized Criticality Phenomenon in Precursors of Gamma-Ray Bursts
Authors: Xiu-Juan Li, Yu-Peng Yang
Figure caption: The size distributions of main bursts. The symbols are the same as those in Figure 1.
Paper: Signatures of the Self-organized Criticality Phenomenon in Precursors of Gamma-Ray Bursts
Authors: Xiu-Juan Li, Yu-Peng Yang
Figure caption: The CDFs of the size differences of main bursts. The symbols are the same as those in Figure 2.
Paper: From Discovery to the First Month of the Type II Supernova 2023ixf: High and Variable Mass Loss in the Final Year before Explosion
Authors: Daichi Hiramatsu, Daichi Tsuna, Edo Berger, Koichi Itagaki, Jared A. Goldberg, Sebastian Gomez, Kishalay De, Griffin Hosseinzadeh, K. Azalee Bostroem, Peter J. Brown, Iair Arcavi, Allyson Bieryla, Peter K. Blanchard, Gilbert A. Esquerdo, Joseph Farah, D. Andrew Howell, Tatsuya Matsumoto, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jaehyon Rhee, Giacomo Terreran, József Vinkó, J. Craig Wheeler
Figure caption: Left: pre-explosion differential flux measurements at the SN 2023ixf position in the ZTF g,r,i bands; ATLAS c,o bands; and WISE W1,W2 bands. Error bars denote 1σ uncertainties, and filled and open symbols are used for detections and 5σ limits, respectively. No significant variability (>5σ) is seen in the ZTF and ATLAS bands, except the two possible ZTF i-band detections. The few sporadic WISE W1 detections are due to imperfect subtraction of the nearby H II region (Figure 1). Right: multiband light curve (top) and U − V color evolution (bottom) of SN 2023ixf. Amateur detections and limits are shown as the open plus signs and downward-pointing triangles, respectively, with no vertical offset. The gray vertical dashed lines mark the epochs of flash spectroscopy (Figure 3). SN 2023ixf is characterized by a rapid rise to the peak with blueward color evolution and a following bright plateau with redward color evolution. (The data used to create this figure will be available upon publication.)(The data used to create this figure are available.)
Paper: From Discovery to the First Month of the Type II Supernova 2023ixf: High and Variable Mass Loss in the Final Year before Explosion
Authors: Daichi Hiramatsu, Daichi Tsuna, Edo Berger, Koichi Itagaki, Jared A. Goldberg, Sebastian Gomez, Kishalay De, Griffin Hosseinzadeh, K. Azalee Bostroem, Peter J. Brown, Iair Arcavi, Allyson Bieryla, Peter K. Blanchard, Gilbert A. Esquerdo, Joseph Farah, D. Andrew Howell, Tatsuya Matsumoto, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jaehyon Rhee, Giacomo Terreran, József Vinkó, J. Craig Wheeler
Figure caption: Comparison of the pseudobolometric light curve of SN 2023ixf with CSM-free light-curve models with varying explosion energies (﹩{E}_{\exp };﹩ top left), and continuous mass-loss light-curve models with a single ﹩{E}_{\exp }﹩ (1.0 × 1051 erg) and CSM velocity (v wind = 115 km s−1): two fixed mass-loss rates (﹩{\dot{M}}_{\mathrm{wind}}﹩) with varying mass-loss durations (t wind;  top right), two fixed t wind with varying ﹩{\dot{M}}_{\mathrm{wind}}﹩ (bottom left), and a zoomed-in version to the early phase (bottom right). The phase is shifted with respect to the Itagaki discovery. CSM-free and minimal-CSM models are unable to reproduce the luminous peak/plateau up to 20 days, and the luminosity excess requires ﹩{\dot{M}}_{\mathrm{wind}}=0.3\mbox{--}1\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩ for t wind = 2 − 1 yr before explosion. The mismatch in the prediscovery excess may suggest a decreasing ﹩{\dot{M}}_{\mathrm{wind}}﹩ toward the explosion.
Paper: From Discovery to the First Month of the Type II Supernova 2023ixf: High and Variable Mass Loss in the Final Year before Explosion
Authors: Daichi Hiramatsu, Daichi Tsuna, Edo Berger, Koichi Itagaki, Jared A. Goldberg, Sebastian Gomez, Kishalay De, Griffin Hosseinzadeh, K. Azalee Bostroem, Peter J. Brown, Iair Arcavi, Allyson Bieryla, Peter K. Blanchard, Gilbert A. Esquerdo, Joseph Farah, D. Andrew Howell, Tatsuya Matsumoto, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jaehyon Rhee, Giacomo Terreran, József Vinkó, J. Craig Wheeler
Figure caption: Spectral time series of SN 2023ixf. The phase of each spectrum with respect to first light is noted on the right side. The prominent flash features of H, He I, He II, C III, C IV, N III, and N IV persist up to 5.6 days, after which a blue featureless continuum dominates the spectra. A transition to a higher ionization state (i.e., C III → C IV) happens during the first two spectra, in line with the blueward U − V color evolution (Figure 2). (The data used to create this figure will be available upon publication.)(The data used to create this figure are available.)
Paper: From Discovery to the First Month of the Type II Supernova 2023ixf: High and Variable Mass Loss in the Final Year before Explosion
Authors: Daichi Hiramatsu, Daichi Tsuna, Edo Berger, Koichi Itagaki, Jared A. Goldberg, Sebastian Gomez, Kishalay De, Griffin Hosseinzadeh, K. Azalee Bostroem, Peter J. Brown, Iair Arcavi, Allyson Bieryla, Peter K. Blanchard, Gilbert A. Esquerdo, Joseph Farah, D. Andrew Howell, Tatsuya Matsumoto, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jaehyon Rhee, Giacomo Terreran, József Vinkó, J. Craig Wheeler
Figure caption: Left: last nondetection (top) and discovery (bottom) images taken by the Itagaki Astronomical Observatory. The red circle marks the position of SN 2023ixf. Right: color-composite (griz-band) image of SN 2023ixf and its host galaxy M101 taken by the Fred Lawrence Whipple Observatory. SN 2023ixf is located on a spiral arm with a nearby H II region roughly at solar metallicity and young (106–107 yr) stellar population (Hu et al. 2018).
Paper: From Discovery to the First Month of the Type II Supernova 2023ixf: High and Variable Mass Loss in the Final Year before Explosion
Authors: Daichi Hiramatsu, Daichi Tsuna, Edo Berger, Koichi Itagaki, Jared A. Goldberg, Sebastian Gomez, Kishalay De, Griffin Hosseinzadeh, K. Azalee Bostroem, Peter J. Brown, Iair Arcavi, Allyson Bieryla, Peter K. Blanchard, Gilbert A. Esquerdo, Joseph Farah, D. Andrew Howell, Tatsuya Matsumoto, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jaehyon Rhee, Giacomo Terreran, József Vinkó, J. Craig Wheeler
Figure caption: Optical light curves of interacting SNe for the eruptive mass-loss model, color-coded by the normalized injected energy, f inj. The dashed and dotted lines are explosions with CSM formed by energy injections 1 and 2 yr before the SN, respectively. The black dashed–dotted lines show the case for the progenitor with no CSM. The green (black) solid lines in the left panels are models with an extended CSM expelled 10 (5) yr before the SN with f inj = 0.3 (0.25). The data points from observations are the same as in Figure 4.
Paper: High-resolution [O I] Line Spectral Mapping of TW Hya Consistent with X-Ray-driven Photoevaporation
Authors: Christian Rab, Michael L. Weber, Giovanni Picogna, Barbara Ercolano, James E. Owen
Figure caption: Comparison of observed [O I] 6300 Å (Simon et al. 2016; Fang et al. 2018, 2023) and [Ne II] 12.8 μm (Pascucci et al. 2011) spectral line profiles to synthetic line profiles of photoevaporative disk wind models. The [O I] line profiles from the models and that observed by Fang et al. (2023) have been degraded to a resolving power R = 40,000, comparable to the resolution in the observation by Simon et al. (2016). For the Fang et al. (2023) data, the error bars correspond to 3σ uncertainties (for visibility). The Gaussian distribution shown in green represents the derived mean centroid shift of −0.8 km s−1 with a standard deviation of 0.4 kms−1 as derived by Fang et al. (2023) from various observations of [O I] 6300 Å. The [Ne II] model profile has been degraded to R = 30,000 and the error bars in the observed profile indicate 1σ uncertainties.
Paper: High-resolution [O I] Line Spectral Mapping of TW Hya Consistent with X-Ray-driven Photoevaporation
Authors: Christian Rab, Michael L. Weber, Giovanni Picogna, Barbara Ercolano, James E. Owen
Figure caption: Comparison of the photoevaporative disk wind model with the observed normalized radial intensity profiles of the [O I] 6300 Å line. The black solid line shows the observation, and the gray solid line shows the PSF (both from Fang et al. 2023). The colored solid and dashed lines show the model results, convolved with the PSF and at the resolution of the model image, respectively. In red, we show the results from the MOCASSIN and in blue from the PRODIMO postprocessing. The inset shows a zoom-in to the region marked by the brown box (r = 1.3–6.4 au) in the main panel.
Paper: High-resolution [O I] Line Spectral Mapping of TW Hya Consistent with X-Ray-driven Photoevaporation
Authors: Christian Rab, Michael L. Weber, Giovanni Picogna, Barbara Ercolano, James E. Owen
Figure caption: [O I] 6300 Å (top) and [Ne II] 12.8 μm (bottom) line flux of our PE disk wind model obtained by multiplying the emissivity with 2π R in order to illustrate the origin of the emission. White solid contour lines indicate the regions where the top 80% of emission originates. White arrows represent the velocity field in the PE model.
Paper: High-resolution [O I] Line Spectral Mapping of TW Hya Consistent with X-Ray-driven Photoevaporation
Authors: Christian Rab, Michael L. Weber, Giovanni Picogna, Barbara Ercolano, James E. Owen
Figure caption: The toy (power-law) model (green) from Fang et al. (2023) compared to results from a radiation thermochemical disk model (purple) without a wind that fits a large set of observational data for TW Hya (Woitke et al. 2019). The dashed and solid colored lines show the radial profiles for the unconvolved and convolved images, respectively. The gray solid line shows the radial profile of the PSF and the black solid line for the [O I] 6300 Å MUSE observations (Fang et al. 2023). The inset shows a zoom-in to the region marked by the brown box (r = 1.3–6.4 au) in the main panel.
Paper: Proton Temperature Anisotropy within the Interplanetary Coronal Mass Ejections Sheath at 1 au
Authors: Zubair I. Shaikh, Anil N. Raghav, Ivan Y. Vasko
Figure caption: 2D distributions of plasma observations in the (β  p∥, T  p⊥/T  p∣∣) plane with hexagonal cells for 333 ICME sheath regions from Wind/SWE data (1995–2015). The color scale is the number of data points per bin in a logarithmic scale. The overplotted black curves present thresholds of different instabilities at different maximum growth rates; γ = 10−2Ω p  (solid), γ = 10−3Ω p  (dashed), and γ = 10−4Ω p  (dotted). Thresholds of proton cyclotron (PCI), mirror mode (MM), parallel firehose (PFH), and oblique firehose (OFH) instabilities are demonstrated as obtained for bi-Maxwellian plasma (Verscharen et al. 2019). The vertical blue dash line corresponds to β  p∥ = 2.
Paper: Proton Temperature Anisotropy within the Interplanetary Coronal Mass Ejections Sheath at 1 au
Authors: Zubair I. Shaikh, Anil N. Raghav, Ivan Y. Vasko
Figure caption: It is a 2D distribution of (β  p∥, T  p⊥/T  p∥) variables with hexagonal cells for 333 ICMEs sheath region from Wind/SWE data (1995–2015). The color scale is the number of data points per bin in a logarithmic scale. The overplotted blue and black curves show the contours of the maximum growth rate (γ  m  = 10−2Ω p  for ζ = 0.5 and ζ = 0) of different instabilities, such as PCI, MM, PFH, and OFH instability, for the bi-Maxwellian plasma. Note that ζ = 0.5 suggests that the contribution of alpha particle temperature instability is included, while ζ = 0 means purely proton temperature anisotropy instability growth rate. The vertical green dash line corresponds to β  p∥ = 2.
Paper: Proton Temperature Anisotropy within the Interplanetary Coronal Mass Ejections Sheath at 1 au
Authors: Zubair I. Shaikh, Anil N. Raghav, Ivan Y. Vasko
Figure caption: Same as Figure 1 but for slow (Vp ≤400  km s−1; top plot), and fast plasma flow (Vp  > 400  km s−1; bottom plot) within the ICME sheath region.