adsabs/AstroCLIMB huggingface dataset:
Paper: Magnetically Driven Neutron-rich Ejecta Unleashed: Global 3D Neutrino–General Relativistic Magnetohydrodynamic Simulations of Collapsars Probe the Conditions for r-process Nucleosynthesis
Authors: Danat Issa, Ore Gottlieb, Brian D. Metzger, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Goni Halevi, Alexander Tchekhovskoy
Figure caption: Gaussian pulse propagating in an optically thin medium at different times. The pulse propagates at the speed of light, and its peak follows a ∝ 1/r2 profile (dashed red line).
Paper: The Case for Edge-on Binaries: An Avenue Toward Comparative Exoplanet Demographics
Authors: Joseph E. Hand, Konstantin Gerbig, Malena Rice
Figure caption: Sky-projected separation of the systems in the final sample, plotted against their distance. Also shown is the angular separation of the stars and their metallicity calculated using isoclassify. Three gray reference lines are shown, representing a 200 au sky-projected separation—indicating the rough (non-sky-projected) binary separation below which exoplanet occurrence is suppressed (M. Moe & K. M. Kratter 2021)—a 1″ angular separation between the two binary components, which roughly corresponds to the ground-based seeing limit imposed by atmospheric turbulence, and a 2″ angular separation, providing a practical RV observability reference (since most precision RV spectrographs have fiber or slit sizes up to ∼1–2″). 39% of the stars in our sample fall between the 1–2″ lines, and an additional 2% fall below the 1″ line. The inset figure in the bottom right shows a Mollweide-projected sky map of the stars in our final sample.
Paper: The Case for Edge-on Binaries: An Avenue Toward Comparative Exoplanet Demographics
Authors: Joseph E. Hand, Konstantin Gerbig, Malena Rice
Figure caption: Simulated exoplanet signals expected for our full edge-on binaries sample. When systems with s < 200 au are excluded from the sample, the distributions are not substantially affected. Left: semiamplitudes of the modeled RV signals as a function of host star mass, assuming three different population-level alignment distributions: perfect alignment (blue), 20°, dispersion (gray), and random/isotropic alignment (red). The contours show the distribution of all models, while the dark lines show the mean RV amplitude within each host mass bin. As expected, the RV amplitude decreases with increasing host star mass. There is a factor of ∼1.6 ×  RV amplitude boost across the full sample between the isotropic alignment scheme, which would be expected for field stars, and the other two alignment schemes, expected for the edge-on binaries in our sample. Right: the expected transit signals from the simulated exoplanet population, assuming the same alignment schemes. The aligned exoplanets are significantly more likely to transit than the isotropically oriented ones, with the perfectly aligned exoplanets being 11.5 times as likely to transit, and the exoplanets matching the observed 20° dispersion being 2.2 times as likely to transit.
Paper: The Case for Edge-on Binaries: An Avenue Toward Comparative Exoplanet Demographics
Authors: Joseph E. Hand, Konstantin Gerbig, Malena Rice
Figure caption: Top: upper and lower asymmetric uncertainties of the system inclinations in our edge-on binaries sample, calculated using lofti_gaia. Bottom: effective temperatures of the stars, calculated from Gaia photometry using isoclassify. The range of temperatures compatible with FGK-type stars is shaded in blue.
Paper: The Case for Edge-on Binaries: An Avenue Toward Comparative Exoplanet Demographics
Authors: Joseph E. Hand, Konstantin Gerbig, Malena Rice
Figure caption: A color–magnitude diagram of stars in the K. El-Badry et al. (2021) binary catalog, including both the primary and secondary stars in each system. The overlaid red points show stars included in our vetted sample of edge-on binaries.
Paper: Evolution of the Three Spectral Components in the Prompt Emission of GRB 240825A
Authors: Chen-Wei Wang, Wen-Jun Tan, Shao-Lin Xiong, Rahim Moradi, Yan-Qiu Zhang, Chao Zheng, Bing Li, Xiao-Bo Li, Cheng-Kui Li, Jia-Cong Liu, Yue Wang, Bo-Bing Wu, Sheng-Lun Xie, Wang-Chen Xue, Shu-Xu Yi, Zheng-Hang Yu, Peng Zhang, Shuang-Nan Zhang, Wen-Long Zhang, Zhen Zhang
Figure caption: The lightcurve of GRB 240825A. (a) The lightcurve of GRB 240825A observed by different missions, along with the corresponding T90. (b) The lightcurve of different energy ranges from keV to MeV observed by GECAM-B. It can be seen that the main pulse actually consists of a soft, slow component, as well as a hard and narrow component. (c) The lightcurve of different energy ranges from keV to GeV. The lightcurves of BGO and LAT are divided into two energy bands based on the dominant spectral components. The profile of the lightcurve in 10–40 MeV exhibits a bump shape, corresponding to the high-energy nonthermal component in the spectrum, which is significantly different from the lightcurve below 10 MeV. (d) The spectral lag of GRB 240825A from keV to GeV, which shows a “positive-to-negative” behavior. All error bars on data points represent their 1σ confidence level.
Paper: Evolution of the Three Spectral Components in the Prompt Emission of GRB 240825A
Authors: Chen-Wei Wang, Wen-Jun Tan, Shao-Lin Xiong, Rahim Moradi, Yan-Qiu Zhang, Chao Zheng, Bing Li, Xiao-Bo Li, Cheng-Kui Li, Jia-Cong Liu, Yue Wang, Bo-Bing Wu, Sheng-Lun Xie, Wang-Chen Xue, Shu-Xu Yi, Zheng-Hang Yu, Peng Zhang, Shuang-Nan Zhang, Wen-Long Zhang, Zhen Zhang
Figure caption: The evolution of the thermal component and the comparison of GRB 240825A with other GRBs. (a) The broken power-law evolution of the thermal component. The flux of the thermal component and soft nonthermal component is calculated in the energy range of 10–1000 keV. (b) Γ obtained by different methods and locations in the Γ0−Eiso diagram. The gray dashed line represents the upper limit of Γ0 by the opacity method. (c) Γph of GRB 240825A obtained by photosphere emission compared with other samples obtained by the same method. (d) The Amati relation of GRB 240825A. (e) The position of GRB 240825A in the T90–fluence diagram. All error bars on data points represent their 1σ confidence level. All shaded areas around the best-fit lines represent their 1σ confidence bands.
Paper: Evolution of the Three Spectral Components in the Prompt Emission of GRB 240825A
Authors: Chen-Wei Wang, Wen-Jun Tan, Shao-Lin Xiong, Rahim Moradi, Yan-Qiu Zhang, Chao Zheng, Bing Li, Xiao-Bo Li, Cheng-Kui Li, Jia-Cong Liu, Yue Wang, Bo-Bing Wu, Sheng-Lun Xie, Wang-Chen Xue, Shu-Xu Yi, Zheng-Hang Yu, Peng Zhang, Shuang-Nan Zhang, Wen-Long Zhang, Zhen Zhang
Figure caption: The time-integrated and time-resolved spectra of GRB 240825A. (a) and (b) The time-integrated spectrum (S-I) of GRB 240825A, including a soft nonthermal component in Band shape, a hard nonthermal component in CPL shape, and a thermal component. The flux is calculated in the energy range from 10 keV to 100 GeV. (c) and (d) The time-resolved spectra (S-II) of GRB 240825A. The thermal component only exists in phases c, d, and e, during which the hard nonthermal component (GeV emission) has not yet appeared. All error bars on data points represent their 1σ confidence level. All shaded areas around the best-fit lines represent their 1σ confidence bands.
Paper: Evolution of the Three Spectral Components in the Prompt Emission of GRB 240825A
Authors: Chen-Wei Wang, Wen-Jun Tan, Shao-Lin Xiong, Rahim Moradi, Yan-Qiu Zhang, Chao Zheng, Bing Li, Xiao-Bo Li, Cheng-Kui Li, Jia-Cong Liu, Yue Wang, Bo-Bing Wu, Sheng-Lun Xie, Wang-Chen Xue, Shu-Xu Yi, Zheng-Hang Yu, Peng Zhang, Shuang-Nan Zhang, Wen-Long Zhang, Zhen Zhang
Figure caption: The flux lightcurves of GRB 240825A. The top panel is the fitting result of the flux lightcurves (based on the spectral fitting result of S-IV spectra) by a multisegment broken power law. The bottom panel is the observed temporal (αt) slopes, which are represented by solid lines, compared with the temporal slopes predicted by the curvature effect (﹩\hat{{\alpha }_{t}}﹩; shown by data points) in different energy ranges. The last segment of the broken power-law evolution of the flux lightcurve in different energy bands roughly conforms to the predictions of high-latitude effects. All error bars on data points represent their 1σ confidence level.
Paper: X-Ray Polarization of the Magnetar 1E 1841−045
Authors: Rachael Stewart, George A. Younes, Alice K. Harding, Zorawar Wadiasingh, Matthew G. Baring, Michela Negro, Tod E. Strohmayer, Wynn C. G. Ho, Mason Ng, Zaven Arzoumanian, Hoa Dinh Thi, Niccolò Di Lalla, Teruaki Enoto, Keith Gendreau, Chin-Ping Hu, Alex van Kooten, Chryssa Kouveliotou, Alexander McEwen
Figure caption: Pure RICS model spectra, without splitting attenuation or cascades, integrated over toroidal volumes as indicated by two ranges of field footpoint altitudes in units of stellar radii, with ﹩{r}_{{\rm{\max }}}\in \{{2}^{3.5},{2}^{4}\}﹩ shown in blue and ﹩{r}_{{\rm{\max }}}\in \{{2}^{1},{2}^{7}\}﹩ in magenta. A blackbody with appropriate area and T = 5 × 106 K is plotted in dotted red. The left and right panels depict viewing angles of θv = {12°, 60°} with respect to the magnetic pole, as indicated. The bottom row depicts the polarization degrees, which trace the ⊥ modes preferentially resulting from scattering, which map to solid and dashed curves in the upper panel. IXPE and NuSTAR data for 1E 1841−045 are plotted, and the energy ranges of the two instruments are indicated with relevant shading. The brown dashed–dotted curve depicts the 2 yr continuum sensitivity for COSI (J. Tomsick et al. 2023).
Paper: X-Ray Polarization of the Magnetar 1E 1841−045
Authors: Rachael Stewart, George A. Younes, Alice K. Harding, Zorawar Wadiasingh, Matthew G. Baring, Michela Negro, Tod E. Strohmayer, Wynn C. G. Ho, Mason Ng, Zaven Arzoumanian, Hoa Dinh Thi, Niccolò Di Lalla, Teruaki Enoto, Keith Gendreau, Chin-Ping Hu, Alex van Kooten, Chryssa Kouveliotou, Alexander McEwen
Figure caption: Top panel: Model photon spectra for O-mode (dashed lines) and X-mode (solid lines) modes from RICS (pink), splitting (purple), and pair synchrotron (green) radiation from a pair cascade from electrons on a closed magnetic field loop with ﹩{r}_{{\rm{\max }}}=6﹩ neutron star radii, surface magnetic field strength B = 32 Bcr, viewing angle, θv = 30°, scattering photons from the whole neutron star surface with temperature 5 × 106 K. Light lines are unattenuated spectra, and dark lines are attenuated (observed) spectra. The normalization is arbitrary. The solid black/red lines are the soft, hard, and total model fits of IXPE/NuSTAR data. The IXPE model has been multiplied by a factor of 1.4 to correct for the calibration uncertainty with NuSTAR. Bottom panel: polarization degree of the total attenuated spectrum.
Paper: IXPE Detection of Highly Polarized X-Rays from the Magnetar 1E 1841-045
Authors: Michela Rigoselli, Roberto Taverna, Sandro Mereghetti, Roberto Turolla, Gian Luca Israel, Silvia Zane, Lorenzo Marra, Fabio Muleri, Alice Borghese, Francesco Coti Zelati, Davide De Grandis, Matteo Imbrogno, Ruth M. E. Kelly, Paolo Esposito, Nanda Rea
Figure caption: IXPE count rate (left panel), polarization degree (central panel), and polarization angle (right panel) as a function of the rotational phase; two cycles are shown for clarity. Results are presented for the 2–8 keV (blue), 2–4 keV (orange), and 4–8 keV (green) energy ranges. Polarization degree and angle are shown for the four phase intervals marked by vertical dotted lines in the left panel. In all the bins where PD is below MDP99, a 3σ upper limit (marked by a downward arrow) is shown for PD and the errors on PA are extended over the entire [−90∘, 90∘] range (double-headed arrows).
Paper: X-Ray Polarization of the Magnetar 1E 1841−045
Authors: Rachael Stewart, George A. Younes, Alice K. Harding, Zorawar Wadiasingh, Matthew G. Baring, Michela Negro, Tod E. Strohmayer, Wynn C. G. Ho, Mason Ng, Zaven Arzoumanian, Hoa Dinh Thi, Niccolò Di Lalla, Teruaki Enoto, Keith Gendreau, Chin-Ping Hu, Alex van Kooten, Chryssa Kouveliotou, Alexander McEwen
Figure caption: The joint spectral νFν models of the simultaneous NuSTAR+IXPE observation. The upper left panel shows the best-fit model of constant∗tbabs(polconst∗bbodyrad+polconst∗powerlaw+polconst∗powerlaw). Note: Only NuSTAR FPMA and DU2 are displayed, to enhance visual clarity. The second left panel shows the data divided by the folded model for the absorbed BB+2PL model; the third, fourth, and bottom left panels show the ratio between the data and the folded model for an absorbed 2BB+PL, 2PL, and BB+PL for comparison. The right panels show the normalized Stokes Q (top) and U (bottom) spectra for the 3 IXPE DUs, with the solid lines showing the best-fit model in linear space. Best-fit spectral parameters can be found in Table 1.
Paper: X-Ray Polarization of the Magnetar 1E 1841−045
Authors: Rachael Stewart, George A. Younes, Alice K. Harding, Zorawar Wadiasingh, Matthew G. Baring, Michela Negro, Tod E. Strohmayer, Wynn C. G. Ho, Mason Ng, Zaven Arzoumanian, Hoa Dinh Thi, Niccolò Di Lalla, Teruaki Enoto, Keith Gendreau, Chin-Ping Hu, Alex van Kooten, Chryssa Kouveliotou, Alexander McEwen
Figure caption: Left: Counts map of the rejected component by the cut devised in A. Di Marco et al. (2023). Middle: Heat maps (with the source region shown in blue shades and the background region in red shades) of the energy fraction contained in the main cluster (EVT_FRA) of the event reconstructed in the detector as a function of the reconstructed energy; the blue line illustrates the background rejection cut, which removes all event below it. Right: FPR and TPR, defined as described in the text, in blue and orange respectively; the dark gray line corresponds to the ratio between the TPR and FPR; the light gray point shows the ratio between the number of counts in the background region and the source region in each energy bin (the ratio is scaled up by 1 for visualization purposes).
Paper: IXPE Detection of Highly Polarized X-Rays from the Magnetar 1E 1841-045
Authors: Michela Rigoselli, Roberto Taverna, Sandro Mereghetti, Roberto Turolla, Gian Luca Israel, Silvia Zane, Lorenzo Marra, Fabio Muleri, Alice Borghese, Francesco Coti Zelati, Davide De Grandis, Matteo Imbrogno, Ruth M. E. Kelly, Paolo Esposito, Nanda Rea
Figure caption: Chandra mosaic of SNR Kes 73. The solid white circles mark the three annular extraction regions for the SNR spectrum, at ﹩{r}_{{\rm{int}}}^{{\rm{SNR}}}=6^{\prime\prime} ﹩ (innermost circle, common to all three) and ﹩{r}_{{\rm{ext}}}^{{\rm{SNR}}}=15^{\prime\prime} ﹩, 48″, and 60″ (outer circles). The dashed magenta circles mark the extraction region used for the background of XMM-Newton, NuSTAR, and IXPE data: ﹩{r}_{{\rm{int}}}^{{\rm{bkg}}}=150^{\prime\prime} ﹩ and ﹩{r}_{{\rm{ext}}}^{{\rm{bkg}}}=240^{\prime\prime} ﹩.
Paper: X-Ray Polarization of the Magnetar 1E 1841−045
Authors: Rachael Stewart, George A. Younes, Alice K. Harding, Zorawar Wadiasingh, Matthew G. Baring, Michela Negro, Tod E. Strohmayer, Wynn C. G. Ho, Mason Ng, Zaven Arzoumanian, Hoa Dinh Thi, Niccolò Di Lalla, Teruaki Enoto, Keith Gendreau, Chin-Ping Hu, Alex van Kooten, Chryssa Kouveliotou, Alexander McEwen
Figure caption: The background-subtracted, phase-averaged polarization characteristics of 1E 1841−045 according to four energy bins. Contours show the 68.3% (1σ) confidence regions for both polarization degree and angle. Stars show the corresponding MDP99 for each energy band. The energy-integrated polarization is shown in dark blue.
Paper: X-Ray Polarization of the Magnetar 1E 1841−045
Authors: Rachael Stewart, George A. Younes, Alice K. Harding, Zorawar Wadiasingh, Matthew G. Baring, Michela Negro, Tod E. Strohmayer, Wynn C. G. Ho, Mason Ng, Zaven Arzoumanian, Hoa Dinh Thi, Niccolò Di Lalla, Teruaki Enoto, Keith Gendreau, Chin-Ping Hu, Alex van Kooten, Chryssa Kouveliotou, Alexander McEwen
Figure caption: Upper Panel: The normalized intensity pulse profile of 1E 1841−045 from 2 to 8 keV using observations from NICER preceding the outburst. Second Panel: The source 2–8 keV intensity pulse profile post-outburst as observed with IXPE. Third Panel: The post-outburst pulse profile from 3 to 10 keV observed simultaneously by NuSTAR. Bottom Panel: The NuSTAR 10–70 keV pulse profile.
Paper: X-Ray Polarization of the Magnetar 1E 1841−045
Authors: Rachael Stewart, George A. Younes, Alice K. Harding, Zorawar Wadiasingh, Matthew G. Baring, Michela Negro, Tod E. Strohmayer, Wynn C. G. Ho, Mason Ng, Zaven Arzoumanian, Hoa Dinh Thi, Niccolò Di Lalla, Teruaki Enoto, Keith Gendreau, Chin-Ping Hu, Alex van Kooten, Chryssa Kouveliotou, Alexander McEwen
Figure caption: Phase-resolved polarization characteristics of 1E 1841−045. The columns display the intensity pulse profiles (top row), polarization degree (center), and polarization angle (bottom row) according to 2–4 keV (left column), 4–8 keV (central column), and 2–8 keV (right column). The phasograms are divided according to five phase bins (shown in colored vertical bands) that correspond to morphological features of the IXPE energy-integrated intensity pulse profile. The corresponding MDP99 for each phase and energy bin are shown as overlapping shaded regions.
Paper: IXPE Detection of Highly Polarized X-Rays from the Magnetar 1E 1841-045
Authors: Michela Rigoselli, Roberto Taverna, Sandro Mereghetti, Roberto Turolla, Gian Luca Israel, Silvia Zane, Lorenzo Marra, Fabio Muleri, Alice Borghese, Francesco Coti Zelati, Davide De Grandis, Matteo Imbrogno, Ruth M. E. Kelly, Paolo Esposito, Nanda Rea
Figure caption: Best fit and residuals to the IXPE (DU1, DU2, and DU3 in black, red, and green, respectively) and NuSTAR (FPMA and FPMB detectors in blue and cyan, respectively) 2024 data. Line code is as in Figure 2.
Paper: IXPE Detection of Highly Polarized X-Rays from the Magnetar 1E 1841-045
Authors: Michela Rigoselli, Roberto Taverna, Sandro Mereghetti, Roberto Turolla, Gian Luca Israel, Silvia Zane, Lorenzo Marra, Fabio Muleri, Alice Borghese, Francesco Coti Zelati, Davide De Grandis, Matteo Imbrogno, Ruth M. E. Kelly, Paolo Esposito, Nanda Rea
Figure caption: Polarization of the single spectral components (see the text for details). Filled and empty contours correspond to the 68% and 99% confidence regions, respectively, around the most probable values; crosses mark the values at which PD and PA were frozen for the specified component.
Paper: IXPE Detection of Highly Polarized X-Rays from the Magnetar 1E 1841-045
Authors: Michela Rigoselli, Roberto Taverna, Sandro Mereghetti, Roberto Turolla, Gian Luca Israel, Silvia Zane, Lorenzo Marra, Fabio Muleri, Alice Borghese, Francesco Coti Zelati, Davide De Grandis, Matteo Imbrogno, Ruth M. E. Kelly, Paolo Esposito, Nanda Rea
Figure caption: Best fit and residuals to the XMM-Newton (EPIC-pn in black and MOS1 and MOS2 in red and green, respectively) and NuSTAR (FPMA and FPMB detectors in blue and cyan, respectively) pre-burst data. The solid lines show the single components of the models, while the dashed lines show the SNR contribution as computed in Section 2.2, which was kept fixed in all fits. The plotted spectra were rebinned to improve visualization, and single components are only displayed in the cases of the EPIC-pn and FPMA detectors for clarity.
Paper: IXPE Detection of Highly Polarized X-Rays from the Magnetar 1E 1841-045
Authors: Michela Rigoselli, Roberto Taverna, Sandro Mereghetti, Roberto Turolla, Gian Luca Israel, Silvia Zane, Lorenzo Marra, Fabio Muleri, Alice Borghese, Francesco Coti Zelati, Davide De Grandis, Matteo Imbrogno, Ruth M. E. Kelly, Paolo Esposito, Nanda Rea
Figure caption: Background-subtracted EPIC-pn pulse profiles in the 2–8 keV (blue), 2–4 keV (orange), and 4–8 keV (green) energy bands (left panel). The three rightmost panels show the NuSTAR pulse profiles in the 2–79 keV (red), 2–8 keV (blue), and 8–79 keV (black) energy bands at three different epochs.
Paper: IXPE Detection of Highly Polarized X-Rays from the Magnetar 1E 1841-045
Authors: Michela Rigoselli, Roberto Taverna, Sandro Mereghetti, Roberto Turolla, Gian Luca Israel, Silvia Zane, Lorenzo Marra, Fabio Muleri, Alice Borghese, Francesco Coti Zelati, Davide De Grandis, Matteo Imbrogno, Ruth M. E. Kelly, Paolo Esposito, Nanda Rea
Figure caption: The normalized Stokes parameters Q/I and U/I measured by the IXPE DU1 (cyan), DU2 (orange), and DU3 (green) along with the combined measurements from the three DUs (black); 1σ error bars are also shown. Dashed circles represent the loci of constant PD while straight lines those of constant PA. The MDP99 relative to the combined measurement is marked by the filled circle.
Paper: IXPE Detection of Highly Polarized X-Rays from the Magnetar 1E 1841-045
Authors: Michela Rigoselli, Roberto Taverna, Sandro Mereghetti, Roberto Turolla, Gian Luca Israel, Silvia Zane, Lorenzo Marra, Fabio Muleri, Alice Borghese, Francesco Coti Zelati, Davide De Grandis, Matteo Imbrogno, Ruth M. E. Kelly, Paolo Esposito, Nanda Rea
Figure caption: Polar plot of the energy-dependent PD and PA obtained using XSPEC (see the text for details). Filled and open contours correspond to the 68% and 99% confidence regions, respectively, around the most probable values reported in Table 3.
Paper: IXPE Detection of Highly Polarized X-Rays from the Magnetar 1E 1841-045
Authors: Michela Rigoselli, Roberto Taverna, Sandro Mereghetti, Roberto Turolla, Gian Luca Israel, Silvia Zane, Lorenzo Marra, Fabio Muleri, Alice Borghese, Francesco Coti Zelati, Davide De Grandis, Matteo Imbrogno, Ruth M. E. Kelly, Paolo Esposito, Nanda Rea
Figure caption: Best fit and residuals to the Chandra spectra of the SNR Kes 73. The three panels show the results for three annular extraction regions centered at (but excluding) 1E 1841−045, as detailed in Section 2.2. The six observations, displayed in black, red, green, blue, cyan, and magenta in increasing order of date, were jointly fit with two VPSHOCK components, shown as solid (hot component) and dashed (soft component) black lines.
Paper: IXPE Detection of Highly Polarized X-Rays from the Magnetar 1E 1841-045
Authors: Michela Rigoselli, Roberto Taverna, Sandro Mereghetti, Roberto Turolla, Gian Luca Israel, Silvia Zane, Lorenzo Marra, Fabio Muleri, Alice Borghese, Francesco Coti Zelati, Davide De Grandis, Matteo Imbrogno, Ruth M. E. Kelly, Paolo Esposito, Nanda Rea
Figure caption: Energy dependence of the linear polarization degree (left panel) and polarization angle (right panel) of the five magnetars observed with IXPE. Thin lines indicate results for the total energy range (in the case of significant polarization detection in the 2–8 keV range). See details in R. Taverna et al. (2022), S. Zane et al. (2023), R. Turolla et al. (2023), and J. Heyl et al. (2024).
Paper: The Striated Solar Photosphere Observed at ﹩0\mathop{.}\limits^{^{\prime\prime} }03﹩ Resolution
Authors: David Kuridze, Friedrich Wöger, Han Uitenbroek, Matthias Rempel, Alexandra Tritschler, Thomas Rimmele, Catherine Fischer, Oskar Steiner
Figure caption: Top: maps of the vertical magnetic flux density, Bz, from the MURaM snapshot at the height z = 0 and Stokes-V amplitude (blue lob) of the spectral line Fe I 630.244 nm (right) normalized to the local continuum intensity. Bottom: G-band intensity, Bz, and Stokes-V profiles along the red and blue lines crossing the dark striae.
Paper: The Striated Solar Photosphere Observed at ﹩0\mathop{.}\limits^{^{\prime\prime} }03﹩ Resolution
Authors: David Kuridze, Friedrich Wöger, Han Uitenbroek, Matthias Rempel, Alexandra Tritschler, Thomas Rimmele, Catherine Fischer, Oskar Steiner
Figure caption: Synthetic G-band intensity profiles along the crosscuts of dark/bright striae marked with red dashes in the top-left simulated G-band image computed for μ = 0.85. Gaussian fits of the individual profiles are overplotted in red.