adsabs/AstroCLIMB huggingface dataset:
Paper: CHAOS. VII. A Large-scale Direct Abundance Study in M33
Authors: Noah S. J. Rogers, Evan D. Skillman, Richard W. Pogge, Danielle A. Berg, Kevin V. Croxall, Jordan Bartlett, Karla Z. Arellano-Córdova, John Moustakas
Figure caption: The abundance trends of α elements observed in M33 relative to the oxygen abundance within the region. Left Column: The relative abundances plotted against R  g /R  e . Right Column: The relative abundances plotted against 12+log(O/H). The weighted average and standard deviation of the relative abundances are also provided as black dashed lines and gray shaded regions, respectively. The number of H II  regions with the specified relative abundance is provided in the lower left corner. The solar abundance ratios from Asplund et al. (2021) are indicated by blue dotted lines and blue shaded regions, respectively. The rows are ordered by increasing atomic number. First Row: log(Ne/O). Second Row: log(S/O). Third Row: log(Cl/O). Fourth Row: log(Ar/O).
Paper: CHAOS. VII. A Large-scale Direct Abundance Study in M33
Authors: Noah S. J. Rogers, Evan D. Skillman, Richard W. Pogge, Danielle A. Berg, Kevin V. Croxall, Jordan Bartlett, Karla Z. Arellano-Córdova, John Moustakas
Figure caption: The direct oxygen abundances in the common H II  regions of M33 measured by CHAOS (black points) and the literature (other colors, same as Figure 7). The best-fit CHAOS gradient and intrinsic dispersion about the gradient are provided as the solid black line and shaded gray region, respectively. The shapes of the points represent the numbers of direct temperatures used to calculate the abundances, as in Figure 4. H II  regions that contain CHAOS abundances but are missing literature abundances are not plotted.
Paper: CHAOS. VII. A Large-scale Direct Abundance Study in M33
Authors: Noah S. J. Rogers, Evan D. Skillman, Richard W. Pogge, Danielle A. Berg, Kevin V. Croxall, Jordan Bartlett, Karla Z. Arellano-Córdova, John Moustakas
Figure caption: A continuum-subtracted Hα image of M33 from Massey et al. (2006) retrieved from NASA/IPAC Extragalactic Database (2019) with the CHAOS slits superimposed on the targeted regions. The R.A. and Decl. are reported on the vertical and horizontal axes, respectively. Left: Hα image of the center of M33. This image encompasses the five MOS fields (red, orange, green, cyan, and purple slits) and four longslit pointings (brown slits). Right: Hα image focused on the far southern portion of M33. Two longslit pointings (brown slits) are provided.
Paper: CHAOS. VII. A Large-scale Direct Abundance Study in M33
Authors: Noah S. J. Rogers, Evan D. Skillman, Richard W. Pogge, Danielle A. Berg, Kevin V. Croxall, Jordan Bartlett, Karla Z. Arellano-Córdova, John Moustakas
Figure caption: Example MODS spectrum of M33+333+745. Temperature-sensitive auroral lines and their model fits (Gaussian plus STARLIGHT continuum) are provided in the subplots. All five commonly employed auroral lines are detected at high S/N. While the spectrum has been corrected for the systemic velocity of M33, the rotational velocity of this extended region has shifted the lines blueward of their theoretical wavelengths (vertical dotted blue lines).
Paper: Rotating Solar Models in Agreement with Helioseismic Results and Updated Neutrino Fluxes
Authors: Wuming Yang
Figure caption: Relative sound-speed and density differences, in the sense (Sun-Model)/Model, between the Sun and models. The solar sound speed and density are given in Basu et al. (2009).
Paper: Rotating Solar Models in Agreement with Helioseismic Results and Updated Neutrino Fluxes
Authors: Wuming Yang
Figure caption: Distributions of observed and predicted ratios r 02 and r 13 as a function of frequency. The circles and triangles show the ratios calculated from the frequencies observed by GOLF & VIRGO (García et al. 2011) and BiSON (Chaplin et al. 1999), respectively.
Paper: Rotating Solar Models in Agreement with Helioseismic Results and Updated Neutrino Fluxes
Authors: Wuming Yang
Figure caption: Left panel: comparison of the Rosseland mean opacities of different models relative to that of a reference model constructed with OPAL opacity tables and Z  s  = 0.0170. Right panel: distributions of the Rosseland mean opacities of the models as a function of radius.
Paper: Rotating Solar Models in Agreement with Helioseismic Results and Updated Neutrino Fluxes
Authors: Wuming Yang
Figure caption: Distributions of hydrogen and metal abundances of models as a function of radius.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Interglitch braking index n ig of PSR J0537−6910 calculated from the spin parameters of each segment between glitches as a function of time since the last glitch. Large and small circles denote NICER and RXTE values, respectively (from here and Antonopoulou et al. 2018; Ho et al. 2020b; Abbott et al. 2021b). Errors in n ig are 1σ. Horizontal dotted lines indicate braking indices n = 3, 5, and 7, which are expected for pulsar spin-down by electromagnetic dipole radiation, gravitational wave–emitting mountain, and gravitational wave–emitting r-mode oscillation, respectively.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Evolution of the spin frequency time derivative ﹩\dot{\nu }﹩ of PSR J0537−6910. ﹩\dot{\nu }﹩ are measured by fitting a timing model to TOAs in each interglitch segment (see Table 4 and Ho et al. 2020b; Abbott et al. 2021b for NICER and Table 1 of Antonopoulou et al. 2018 for RXTE). Errors are the 1σ uncertainty. Dashed line shows a linear fit of NICER and RXTE data with the best-fit ﹩\ddot{\nu }=-7.92\times {10}^{-22}\,\mathrm{Hz}\,{{\rm{s}}}^{-2}﹩.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Pulsar spin period P and spin period time derivative ﹩\dot{P}﹩. Circles denote pulsars whose values are taken from the ATNF Pulsar Catalogue (Manchester et al. 2005; version 1.66), and stars indicate pulsars considered in this work (see Table 1). Dashed lines indicate characteristic age ﹩{\tau }_{{\rm{c}}}\equiv P/2\dot{P}﹩, and dotted lines indicate magnetic field strength ﹩B=3.2\times {10}^{19}\,{\rm{G}}{\,(P\dot{P})}^{1/2}﹩.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Glitch Δν (top) and ﹩{\rm{\Delta }}\dot{\nu }﹩ (bottom) as functions of time (see Table 5 and Ho et al. 2020b; Abbott et al. 2021b). Errors in ﹩{\rm{\Delta }}\dot{\nu }﹩ are the 1σ uncertainty.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Timing residuals of PSR J0058−7218 from a best fit of NICER pulse TOAs using the timing model given in Table 3. Errors are 1σ uncertainty.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Pulse profile of PSR J0058−7218 from 153 ks of NICER data at 0.8–5 keV. Errors are 1σ uncertainty. Two rotation cycles are shown for clarity.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Schematic of a glitch (see also Ray et al. 2019). The pulsar spin frequency ν (solid line) is observed to decrease at a rate ﹩\dot{\nu }﹩, due to energy loss from electromagnetic radiation, while a superfluid component within the star rotating at ν sf is pinned and does not spin down with the rest of the star (﹩{\dot{\nu }}_{\mathrm{sf}}=0;﹩ dashed line). When the superfluid component unpins and couples to the nonsuperfluid component after time T g, the superfluid transfers angular momentum (∝ Δν sf) to the rest of the star, and a spin-up glitch Δν is observed. The pulsar then continues to spin down when the superfluid becomes pinned again.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Spin frequency ν of PSR J1813−1749 (top) and the difference between the best-fit linear model and data (bottom) as functions of time. Measurements of ν are made using XMM-Newton (triangles), Chandra (squares), Green Bank Telescope in radio (stars), NuSTAR (cross), and NICER (circle). Dashed line shows a linear fit of all ν measurements with best-fit ﹩\dot{\nu }=-6.3442\times {10}^{-11}\,\mathrm{Hz}\,{{\rm{s}}}^{-1}﹩.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Pulse profile of PSR J1101−6101 from 370 ks of NICER data at 1.5–10 keV (top), while lower panels show pulse profiles from 136 ks of NuSTAR data at 1.6–10 , 10–20 , 20–60,  and 1.6–60 keV. Errors are 1σ uncertainty. Two rotation cycles are shown for clarity.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Correlation between time interval to the next glitch ΔT and size of glitch Δν of PSR J0537−6910. Large and small circles denote NICER and RXTE values, respectively (from here and Antonopoulou et al. 2018; Ho et al. 2020b; Abbott et al. 2021b). Errors in Δν are 1σ. The vertical dotted line indicates the size of NICER glitch 15, which is the most recent glitch (on 2021 November 4) and for which time to next glitch is not known yet. Dashed line shows the linear fit result ΔT = 49.2  d (Δν/10 μHz) + 25 d.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Fractional glitch magnitude Δν/ν of PSR J0537−6910 shown as a cumulative sum over each previous glitch. RXTE values are from Table 2 of Antonopoulou et al. (2018). Dashed line indicates a line with a slope of 8.918 × 10−7 yr−1, which is the glitch activity A g ≡ ∑ i (Δν/ν) i /T obs, where T obs is the time over which the pulsar is monitored. NICER values are offset by Δν/ν = 16.7 × 10−6, which is the extrapolated value of the RXTE-only glitch activity at the epoch of NICER segment 0 at MJD 58,020.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Pulse profiles of PSR J1101−6101 from Fermi LAT data at 0.3–3 GeV (solid histogram) and from NICER data at 1.5–10 keV (dashed curve with arbitrary normalization; see also Figure 10). Errors are 1σ uncertainty. Two rotation cycles are shown for clarity.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Timing residuals of PSR J1412+7922 from a best fit of NICER pulse TOAs with the timing model given in Table 7. Errors are 1σ uncertainty.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Timing residuals of PSR J1849−0001 from a best fit of NICER (circles) and one Swift (cross) pulse TOAs, with the timing model given in Table 9. Errors are 1σ uncertainty.
Paper: Timing Six Energetic Rotation-powered X-Ray Pulsars, Including the Fast-spinning Young PSR J0058-7218 and Big Glitcher PSR J0537-6910
Authors: Wynn C. G. Ho, Lucien Kuiper, Cristóbal M. Espinoza, Sebastien Guillot, Paul S. Ray, D. A. Smith, Slavko Bogdanov, Danai Antonopoulou, Zaven Arzoumanian, Michał Bejger, Teruaki Enoto, Paolo Esposito, Alice K. Harding, Brynmor Haskell, Natalia Lewandowska, Chandreyee Maitra, Georgios Vasilopoulos
Figure caption: Timing residuals of PSR J1101−6101 from a best fit of NICER pulse TOAs with the timing model given in Table 6. Errors are the 1σ uncertainty.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: The plane of 5 GHz radio luminosity (L radio) vs. 1–10 keV X-ray luminosity (L X), with points representing X-ray binaries (accreting neutron stars, black holes), accreting and transitional millisecond pulsars, flaring CVs, classical novae, and classical symbiotics in outburst. The green shaded box represents the range of luminosities of classical novae. The classical symbiotics Z And and AG Dra are represented with black and red stars, respectively, while the X-ray binary V Sge is represented with a cyan star. The radio luminosity of V1047 Cen at 5 GHz is plotted with a dashed blue horizontal line and is calculated assuming a flat spectrum. Adopted from Bahramian et al. (2018) https://zenodo.org/record/1252036/export/hx.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: Optical spectral evolution of V1047 Cen. The numbers in brackets are days since t 0.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: Line profile evolution of Hβ throughout the outburst of V1047 Cen. The numbers between brackets are days after outburst. The red dashed lines represent the rest velocity (V vrad = 0 km s−1). A heliocentric correction is applied to the radial velocities.
Paper: Magnetic Field Structure, Doppler Shift, and Intensity of Active Regions and Their Connections with the Solar Wind
Authors: Chi Ma, Hui Fu, Zhenghua Huang, Lidong Xia, Jinmei Zheng, Xinzheng Shi, Bo Li
Figure caption: Remote sensing of AR 10987 and its associated solar wind. The full-disk image taken by EIT 195 Å and the subregion map inside the rectangle (outline of the region scanned by EIS) are presented in (a) and (b), the photospheric magnetic field measured by MDI is given in (c), the EIS Fe XII 195.12 Å intensity and Doppler maps of AR 10987 are shown in panels (d) and (e), the parameters of the solar wind are shown in (f). The red and blue crosses represent the footpoints of the open magnetic field lines derived from the PFSS model. The sky-blue lines contour the magnetically concentrated area and the red lines outline the footpoint areas of blueshift.
Paper: Genesis and Coronal-jet-generating Eruption of a Solar Minifilament Captured by IRIS Slit-raster Spectra
Authors: Navdeep K. Panesar, Sanjiv K. Tiwari, Ronald L. Moore, Alphonse C. Sterling, Bart De Pontieu
Figure caption: Schematic of the possible arrangement, action, and reconnection of the magnetic field in and around the minifilament before and during the jet-generating blowout eruption of the minifilament-carrying fields. The view direction is from the southwest, more or less along the direction of the flux-cancelation PIL underlying the minifilament seen in Figure 2(a) and more or less orthogonal to the jet spire seen in Figure 2(e). The horizontal black line is the solar surface. Positive and negative magnetic flux polarities are labeled with “+” and “–” signs, respectively. Each red X marks a site of ongoing magnetic field reconnection. The minifilament’s cool plasma and reconnected magnetic field lines are sky blue and red, respectively. The thick sky blue arrow in panel (c) is the jet spire and the elliptical arrow shows the clockwise rotation (the head of the elliptical arrow is closer to the viewer than the tail). Panel (a) shows the setup before the eruption. The black slanted bar marks the location of current-sheet formation at the magnetic null point between the flux-rope-enveloping lobe and ambient far-reaching field. Panel (b) is early in the slow rise of the erupting minifilament-carrying flux rope and enveloping lobe, when reconnection of the outside of the lobe has started but the erupting flux rope has not yet kinked. In panel (c), the erupting minifilament flux rope has kinked (writhed) to give some of its right-handed magnetic twist to a right-handed writhe.
Paper: Genesis and Coronal-jet-generating Eruption of a Solar Minifilament Captured by IRIS Slit-raster Spectra
Authors: Navdeep K. Panesar, Sanjiv K. Tiwari, Ronald L. Moore, Alphonse C. Sterling, Bart De Pontieu
Figure caption: Thermal and dynamical properties of the minifilament eruption. Panels (a) and (e), (b) and (f), and (c) and (g) show the maps of temperature, LOS velocity (V LOS), and electron density (log(n  e )), respectively, evaluated at log(τ) = −4.2. Panels (d) and (h) show the spectroheliograms of the Mg II k line at 2796.38 Å. The black and white arrows in (a)–(c) point to the JBP. In panel (f) the upper black arrow points to the weak redshifts and the lower arrow to the blueshifts along the jet spire.
Paper: Genesis and Coronal-jet-generating Eruption of a Solar Minifilament Captured by IRIS Slit-raster Spectra
Authors: Navdeep K. Panesar, Sanjiv K. Tiwari, Ronald L. Moore, Alphonse C. Sterling, Bart De Pontieu
Figure caption: Jet speed. Panels (a) and (c) show a spectroheliogram of the Mg II k line and an AIA 171 Å image of the jet. The diagonal arrows in (a) and (c) show the cut for the time–distance maps plotted in (b) and (d). Panels (b) and (d) show the time–distance maps from the cuts in Figures 7(a) and (c). Map (b) shows the progression of the tip of the dark jet spire in panel (a); map (d) shows the progression of the bright tip of the dark jet spire in panel (c). The dotted lines in (b) and (d) are the paths used to calculate the speed of plasma outflows along the jet spire. The dotted–dashed line in (d) marks the upper edge of the dark minifilament during the minifilament’s slow rise. The cyan arrow in (d) points to the remote brightening that appears to the east of the erupting minifilament.
Paper: Magnetic Field Structure, Doppler Shift, and Intensity of Active Regions and Their Connections with the Solar Wind
Authors: Chi Ma, Hui Fu, Zhenghua Huang, Lidong Xia, Jinmei Zheng, Xinzheng Shi, Bo Li
Figure caption: Remote sensing of AR 10961 and its associated solar wind. The full-disk image taken by EIT 195 Å and the subregion map inside the rectangle (outline of the region scanned by EIS) are presented in (a) and (b), the photospheric magnetic field measured by MDI is given in (c), EIS Fe XII 195.12 Å intensity and Doppler maps of AR 10961 are shown in panels (d) and (e), the parameters of the solar wind are shown in (f). The red and blue crosses represent the footpoints of open magnetic field lines derived from the PFSS model. The sky-blue lines contour the MCA and the red lines outline the footpoint areas of blueshift.