adsabs/AstroCLIMB huggingface dataset:
Paper: A Systematic Survey of Moon-forming Giant Impacts. I. Nonrotating Bodies
Authors: Miles Timpe, Christian Reinhardt, Thomas Meier, Joachim Stadel, Ben Moore
Figure caption: Successful cases according to a set of permissive (M  d  ≥ M ☾ and ﹩{F}_{d}^{\mathrm{Fe}}\leqslant 0.04﹩) and strict (2 M ☾ ≤ M  d  ≤ 4 M ☾, ﹩{F}_{d}^{\mathrm{Fe}}\leqslant 0.02﹩, and ∣δ pd∣ ≤ 0.05) constraints. These results show that nonrotating collisions cannot generate favorable disk properties while simultaneously reproducing the current Earth–Moon angular momentum budget. If the angular momentum constraint is relaxed, then only a handful of collisions can meet the remaining constraints, including a sufficiently massive protolunar disk mass, a disk iron fraction of less than 2%, and a difference in post-impact composition of the Earth and protolunar disk of less than 5%. The distribution of these cases suggests that the most promising case of impacts are low-velocity, high-angular-momentum impacts between near-equal-mass bodies.
Paper: A Systematic Survey of Moon-forming Giant Impacts. I. Nonrotating Bodies
Authors: Miles Timpe, Christian Reinhardt, Thomas Meier, Joachim Stadel, Ben Moore
Figure caption: The disk-finding algorithm differentiates the post-impact planet (i.e., the proto-Earth) from the circumplanetary disk and ejecta. It identifies the radius of the planet by finding the radius at which the median rotation rate of local particles deviates significantly from the expected rotation rate (roughly corresponding to the solid-body rotation rate).
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: (a) PPD-corrected 3–9 keV PG with m = 4, using E b = 10 keV and R ppd = 62 deg keV−1. Like in Figure 1(b), the orbital parameters except e are varied at each P. A vertical green line indicates P NS of Equation (1). (b) Details of (a) around the peak, shown over the same period range as in Figure 1(b). The dashed black line gives the PPD-uncorrected PG, and orange is the difference between blue and black. (c) Same as (b) but in 3–30 keV. The blue trace employs E b = 10.4 keV and R ppd = 64. The red curve shows a result when R ppd is also allowed to float (with E b still fixed) at each P, from −90 to 90 with a step of 1.0.
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: Stage 3 results from the GIS. (a) PGs with m = 4 in 2.8–12 keV, calculated over a broad period range with Δ P = 100 μs, using the PPD correction in which R ppd is optimized at each P (see text). Black, green, red, blue, and gray correspond to ﹩{\dot{P}}_{7}=0.7,0.8,0.9,1.0﹩ and 1.1, respectively. (b), (c), and (d) show results over a limited period range, using Δ P = 20 μs, for ﹩{\dot{P}}_{7}=0.9,0.75,﹩ and 1.05, respectively. (e) and (f) give details of the ﹩{P^{\prime} }_{2}﹩ peak in (d) and the ﹩{P}_{1}^{\prime} ﹩ peak in (b), respectively, where the blue trace presents the optimum R ppd. (g) Superposition of the ﹩{P}_{1}^{\prime} ﹩ peaks for six values of ﹩\dot{P}﹩ (given in color), which cover the range of Equation (6).
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: (a) Pulse profiles of LS 5039 with the ASCA GIS, in 2.8–3.6 keV (red), 3.6–5.0 keV (green), 5–12 keV (blue), and 2.8–12 keV (black). They are all orbit-corrected and folded at P fin. (b) Same but further corrected for the PPD effect, except in 1.0–2.8 keV (dashed purple). (c) Comparison between the GIS (2.8–12 keV; red) and NuSTAR (10–30 keV; blue) pulse profiles. Except for the binning, they are identical to the black histograms in Figure 12(b) and Figure 1(d), respectively. The GIS profile is rescaled (see the main text) and shown with finer bins than in (b).
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: Final (Stage 4) PGs from the 2.8–12 keV GIS data, in which ﹩{a}_{{\rm{x}}}\sin i﹩, ω, and τ 0 are readjusted at each P, whereas the PPD parameters are fixed (see text). The red and green traces show the maximum ﹩{Z}_{4}^{2}﹩ and the optimum τ 0, respectively. (a) Result for SOL-1, assuming e = 0.306, E b = 10.0 keV, and R ppd = −23.4. (b) Result for SOL-2, using e = 0.306, E b = 10.5 keV, and R ppd = −62. (c) Same as (a), but employing e = 0.278 (from Suzaku), together with E b = 10.1 keV and R ppd = −23.6.
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: Comparison of the orbital constraints in 10–30 keV (solid lines) and 3–9 keV (dashed lines; E b = 10 keV and R ppd = 62 fixed). The values of P, ﹩{a}_{{\rm{x}}}\sin i﹩, and ω, which maximize ﹩{Z}_{4}^{2}﹩, are shown as a function of τ 0, together with ﹩{Z}_{4}^{2}﹩. The ranges over which these quantities are scanned are indicated by arrows along the ordinates. The lines denoted as comparison are explained in the main text. (a) ﹩{Z}_{4}^{2}﹩ (red) and ﹩{a}_{{\rm{x}}}\sin i﹩ (blue). (b) ω (green) and P (brown).
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: Same as Figure 3(b) but for the 2.8–12 keV GIS data in Stage 3. The R ppd dependence of ﹩{Z}_{4}^{2}﹩ is shown for three values of ﹩{\dot{P}}_{7};﹩ 0.80 (green), 0.88 (red), and 0.95 (dashed purple). At each R ppd, P is scanned over 8.8860 ± 0.0015 s, and its optimum value for ﹩{\dot{P}}_{7}=0.88﹩ is presented in blue (right ordinate). In all cases, E b = 10 keV is retained.
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: An m = 2 PG from the 6–12 keV GIS data in Stage 1, generated without orbital corrections. The inset shows an expansion leftward of the peak at P = P 0 = 8.8820 s. The green arrow represents Equation (4).
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: Summary of the period estimates with ASCA, superposed on the radial X-ray Doppler curve from the Suzaku (red) and NuSTAR (blue) solutions. The periods and period differences are all shown in units of ms. The periods found in Stages 1–4 are indicated by circled numbers. The orbital phase covered with ASCA is indicated in green, and the optimum ﹩{\dot{P}}_{7}﹩ by a dotted black line.
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: Stage 2 results from the GIS: epoch folding of the 5.3–12 keV GIS data with m = 4, incorporating ﹩\dot{P}﹩. (a) Color map of ﹩{Z}_{4}^{2}﹩ on a ﹩(P,\dot{P})﹩ plane. (b) Cross section of (a) at ﹩{\dot{P}}_{7}=0.7﹩ (dashed cyan line). (c) The same but at ﹩{\dot{P}}_{7}=0.9﹩ (dashed orange line).
Paper: Simultaneous Estimates of Star-cluster Age, Metallicity, Mass, and Extinction (SESAMME). I. Presenting an MCMC Approach to Spectral Stellar Population Fitting
Authors: Logan H. Jones, Svea Hernandez, Linda J. Smith, Bethan L. James, Alessandra Aloisi, Søren Larsen
Figure caption: Visualization of the format of a SESAMME model cube, generated from BPASS v2.3 models with binary physics and a solar α/Fe, in the form of Astropy Tables. Within each slice of the model cube, the first column gives the wavelength grid (which, in this case, has been truncated to only cover the rest-frame UV), while the remaining columns give the light output at a fixed log(age) at each wavelength bin in units of L ⊙ Å−1. For clarity, only the first 10 age intervals and three of the 13 possible metallicities in BPASS are shown.
Paper: The Metallicity and Distance of Leo A from Blue Supergiants
Authors: Miguel A. Urbaneja, Fabio Bresolin, Rolf-Peter Kudritzki
Figure caption: The sHRD of the BSGs in Leo A, together with MESA stellar evolution tracks calculated for [Z] = −1.25 (Choi et al. 2016; Dotter 2016). The tracks include the effects of stellar rotation and are calculated for initial main-sequence masses of 5 (short-dashed), 7 (solid), 10 (long-dashed), and 15 (dashed–dotted) M ⊙.
Paper: The Metallicity and Distance of Leo A from Blue Supergiants
Authors: Miguel A. Urbaneja, Fabio Bresolin, Rolf-Peter Kudritzki
Figure caption: Determination of temperature and metallicity from Δχ 2 isocontours obtained through the comparison of observed and synthetic spectra (see text). Plotted are Δχ 2 = 3 (red), 6 (blue), and 9 (black) and the final fit values (red dot). The red and black isocontours correspond to the 1σ and 2σ uncertainties, respectively. Top: target 10. Middle: target 11. Bottom: target 04.
Paper: The Metallicity and Distance of Leo A from Blue Supergiants
Authors: Miguel A. Urbaneja, Fabio Bresolin, Rolf-Peter Kudritzki
Figure caption: Balmer line fit of target 04 of Table 1. The blue curve shows the gravity log g at which the best fit of the Balmer lines is obtained for each value of T eff on the abscissa. The red square shows the final log g and T eff values following from the additional fit of the metal lines along this curve (see text). The final log g and T eff for all targets analyzed are given in Table 2.
Paper: The Metallicity and Distance of Leo A from Blue Supergiants
Authors: Miguel A. Urbaneja, Fabio Bresolin, Rolf-Peter Kudritzki
Figure caption: Targets 11 (top row of each panel) and 04 (bottom row) observed metal lines (black) fit with the synthetic spectrum calculated for the final stellar parameters (red) in selected parts of the spectrum.
Paper: The Metallicity and Distance of Leo A from Blue Supergiants
Authors: Miguel A. Urbaneja, Fabio Bresolin, Rolf-Peter Kudritzki
Figure caption: Target 10 observed metal lines (black) fit with the synthetic spectrum calculated for the final stellar parameters (red) in selected parts of the spectrum.
Paper: The Metallicity and Distance of Leo A from Blue Supergiants
Authors: Miguel A. Urbaneja, Fabio Bresolin, Rolf-Peter Kudritzki
Figure caption: Compilation of the spectra of the 12 targets observed.
Paper: The Metallicity and Distance of Leo A from Blue Supergiants
Authors: Miguel A. Urbaneja, Fabio Bresolin, Rolf-Peter Kudritzki
Figure caption: Balmer line fit of target 04 using the adopted T eff, log g, and [Z] values in Table 2. The model (red) and observed (black) Balmer line profiles are compared. The abscissa is the displacement from the line center in angstroms.
Paper: The Metallicity and Distance of Leo A from Blue Supergiants
Authors: Miguel A. Urbaneja, Fabio Bresolin, Rolf-Peter Kudritzki
Figure caption: Identification of the spectroscopic targets in a Subaru B-band image of Leo A taken from Stonkutė et al. (2014).
Paper: Nature of Turbulence inside Small-scale Magnetic Flux Ropes near the Sun: Parker Solar Probe Observations
Authors: Zubair I. Shaikh, Geeta Vichare, Ankush Bhaskar, Anil N. Raghav, Sofiane Bourouaine
Figure caption: The top panel shows FFT-based power spectral density of magnetic field data during the passage of SSMFRs as a function of the spacecraft frequency. The red dashed line shows power-law fitting (95% confidence bound) during the frequency interval from 20 mHz to 2 Hz. The bottom panel represents a plot of magnetic helicity σ  m  (gray colored plot; as per Equation (1)) as a function of the spacecraft frequency (where the overplotted black plot is a smoothed version of the gray plot). The vertical red dashed line denotes the ion (proton) cyclotron frequency (f  ci ), whereas the vertical blue and black dashed lines denote the frequency corresponding to the ion inertia length (f  di ) and ion Larmor radius (f  Li ), respectively.
Paper: Nature of Turbulence inside Small-scale Magnetic Flux Ropes near the Sun: Parker Solar Probe Observations
Authors: Zubair I. Shaikh, Geeta Vichare, Ankush Bhaskar, Anil N. Raghav, Sofiane Bourouaine
Figure caption: Temporal profile of plasma parameters and magnetic field during SSMFRs observed by the PSP spacecraft dated 2019 August 23. The top panels (first, second, and third) represent total IMF (B mag), IMF components (B vec = (BR, BT, and BN)), and IMF azimuth (ϕ) and elevation (θ) angles, respectively. The fourth, fifth, and sixth panels show the variation in plasma speed (Vp), density (Np), and temperature (T), respectively. The last two panels show variations of thermal (Pth) and magnetic (Pmag) pressures.
Paper: The Metallicity and Distance of Leo A from Blue Supergiants
Authors: Miguel A. Urbaneja, Fabio Bresolin, Rolf-Peter Kudritzki
Figure caption: Mass–metallicity relationship of star-forming galaxies based on absorption line studies of the young stellar population. Results from BSGs are shown in blue, while metallicities from red supergiants (RSGs) and superstar clusters (SSCs) are displayed in red. The yellow symbols correspond to the recent population synthesis study of 250,000 star-forming SDSS galaxies by Sextl et al. (2023). Our new result obtained for Leo A is represented with the star symbol. Predictions from the galaxy evolution look-back models by Kudritzki et al. (2021) are shown as the green curve.
Paper: The Metallicity and Distance of Leo A from Blue Supergiants
Authors: Miguel A. Urbaneja, Fabio Bresolin, Rolf-Peter Kudritzki
Figure caption: Stellar evolution FGLR at [Z] = −1.25 constructed from Figures 8 and 11 for BSGs in the first crossing phase toward the red giant phase (red) and during the blue loop phase (blue). The FGLR plotted in dark red, also obtained from MESA evolutionary tracks, refers to the first crossing phase at [Z] = −0.25.
Paper: Nature of Turbulence inside Small-scale Magnetic Flux Ropes near the Sun: Parker Solar Probe Observations
Authors: Zubair I. Shaikh, Geeta Vichare, Ankush Bhaskar, Anil N. Raghav, Sofiane Bourouaine
Figure caption: Histogram plot of the 44 SSMFR turbulent parameters: spectral index (α; top panel), absolute magnetic helicity (∣σ  m ∣;  bottom left panel), and compressibility (C; bottom right panel). The "Std" implies standard deviation.
Paper: The Metallicity and Distance of Leo A from Blue Supergiants
Authors: Miguel A. Urbaneja, Fabio Bresolin, Rolf-Peter Kudritzki
Figure caption: The HRD of the MESA stellar evolution tracks calculated for [Z] = −1.25 (Choi et al. 2016; Dotter 2016). The tracks include the effects of stellar rotation and are calculated for initial main-sequence masses of 5 (short-dashed), 7 (solid), 10 (long-dashed), and 15 (dashed–dotted) M ⊙.
Paper: Nature of Turbulence inside Small-scale Magnetic Flux Ropes near the Sun: Parker Solar Probe Observations
Authors: Zubair I. Shaikh, Geeta Vichare, Ankush Bhaskar, Anil N. Raghav, Sofiane Bourouaine
Figure caption: Spectral index estimation for Figure 1 (in the main text) but with linear fitting to log10(f) vs. log10(PSD) in the frequency ranges (1) 3–30 mHz, and (2) 50 mHz–1.0 Hz. We highlighted the data points during the fitting interval for better visibility.
Paper: X-Ray, Near-ultraviolet, and Optical Flares Produced by Colliding Magnetospheres in the Young High-eccentricity Binary DQ Tau
Authors: Konstantin V. Getman, Ágnes Kóspál, Nicole Arulanantham, Dmitry A. Semenov, Grigorii V. Smirnov-Pinchukov, Sierk E. van Terwisga
Figure caption: NuSTAR and Swift light curves and related temporal evolution of the X-ray median energy. The error bars indicate the 68% confidence intervals for all the shown quantities. (a) The background-subtracted light curve for the combined FPMA and FPMB NuSTAR data is shown in red. The solid red curves show the best-fit exponential fits to the rise and decay phases of the main flare and to the decay phase of the second flare. The dashed gray curves indicate exponential fits for the rise and decay phases of the third flare. The Swift-XRT data, with each point corresponding to a single observation, are displayed in black. The NuSTAR count rate is scaled by a factor of ×3 to match the Swift count rate level. The average lowest NuSTAR+Swift-XRT count rate level across the entire observed periastron phase and the peak level of the main flare are marked by the black dashed lines. (b) The temporal evolution of the X-ray median energy is shown for both the NuSTAR (red) and Swift (black) data. (c, d) Swift-UVOT light curves are provided for the six UVOT filters. Polynomial and linear fits to the initial and final segments of the flare light curves, created using the R function lm, are depicted by the dashed and dotted colored lines, respectively. These fits serve as potential baselines for the UVOT flaring resulting from magnetic reconnection.
Paper: X-Ray, Near-ultraviolet, and Optical Flares Produced by Colliding Magnetospheres in the Young High-eccentricity Binary DQ Tau
Authors: Konstantin V. Getman, Ágnes Kóspál, Nicole Arulanantham, Dmitry A. Semenov, Grigorii V. Smirnov-Pinchukov, Sierk E. van Terwisga
Figure caption: The Chandra light curve and the related temporal evolution of the X-ray median energy. Each point represents a single Chandra observation, and the error bars indicate the 68% confidence intervals for all the shown quantities. (a) On the shown light curve, the dashed gray line marks the characteristic level of the X-ray emission in DQ Tau. The point with the highest count rate corresponds to the ObsID 26471, and this count rate value is not corrected for pileup. The dashed black line connects the two points corresponding to ObsIDs 26471 and 26472 and indicates the exponential decay of the X-ray emission assuming that these points are associated with the same large X-ray flare. (b) The evolution of the X-ray median energy is displayed. The dashed gray line and gray error bar mark the median level of the energy and its 68% uncertainty for the data comprising all but one observation (ObsID 26471 with the highest count rate and median energy values).
Paper: X-Ray, Near-ultraviolet, and Optical Flares Produced by Colliding Magnetospheres in the Young High-eccentricity Binary DQ Tau
Authors: Konstantin V. Getman, Ágnes Kóspál, Nicole Arulanantham, Dmitry A. Semenov, Grigorii V. Smirnov-Pinchukov, Sierk E. van Terwisga
Figure caption: NuSTAR, Swift, and Chandra images of DQ Tau and its neighborhood. The color map, ranging from yellow to red to blue, indicates the intensity of X-rays, with yellow and blue pixels representing more and less X-ray counts, respectively. Each panel has its own unique intensity scale. DQ Tau source extraction regions are marked by the green circles. (a) ﹩13^{\prime} \times 13^{\prime} ﹩ image from the merged NuSTAR FPMA+FPMB event lists in the 3–10 keV energy band. (b) Same as panel (a), but in the 10–50 keV energy band. (c) ﹩7^{\prime} \times 7^{\prime} ﹩ Swift-XRT cutout of DQ Tau’s neighborhood in the 0.2–10 keV band, which was obtained from the merged event lists of the 16 Swift observations. The other two X-ray objects visible in this image are the young stellar systems Haro 6-37 A,B and DR Tau, located to the northeast and southeast of DQ Tau, respectively. (d) ﹩1^{\prime} \times 1^{\prime} ﹩ Chandra-ACIS-I3 cutout in the 0.5–8 keV band centered on DQ Tau. This image was obtained from the merged event lists of the 12 Chandra observations.
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: Comparison of the χ r and Z  m  2 statistics. (a) The orbit-corrected NuSTAR PGs in 10–30 keV, calculated by ﹩{Z}_{4}^{2}﹩ (blue) and χ r (brown; ν = 19). (b) The maximum Z  m  2 (black) from the 10–30 keV NuSTAR data, is shown as a function of m. The associated ﹩{{ \mathcal P }}_{\mathrm{ch}}^{(1)}﹩ is given in orange, where the vertical brown arrow indicates typical values obtained with χ r. (c) A scatter plot between χ r and ﹩{Z}_{4}^{2}﹩, for the results in panel (a), Table 1, and Table 3. The white box with black bars indicates the average and standard deviation for white noise. The values of ﹩{{ \mathcal P }}_{\mathrm{ch}}^{(1)}﹩ are shown in orange.
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: Upper probability distributions of ﹩{Z}_{4}^{2}﹩ values from the control studies using off-peak period ranges. At each period, the PPD correction is incorporated, with R ppd allowed to vary freely in the same manner as for the pulse-period search. See the main text (Appendix C) for details. The target values are indicated by vertical green line segments. (a) For the 3–30 keV NuSTAR data incorporating the orbital and PPD corrections, with E b = 10.4 fixed. (b) For the 2.8–12 keV GIS data in Stage 3, assuming E b = 10 keV.
Paper: X-Ray, Near-ultraviolet, and Optical Flares Produced by Colliding Magnetospheres in the Young High-eccentricity Binary DQ Tau
Authors: Konstantin V. Getman, Ágnes Kóspál, Nicole Arulanantham, Dmitry A. Semenov, Grigorii V. Smirnov-Pinchukov, Sierk E. van Terwisga
Figure caption: Simultaneous fitting of the Swift and NuSTAR X-ray spectra. The Swift-XRT spectrum (shown in green) is merged from the data of all 16 Swift snapshots covering the 0.9–1.22 orbital phase range. The NuSTAR FPMA (black) and FPMB (red) spectra are from the data of the entire NuSTAR observation that spans the 0.9–1.15 phase range. The best-fit optically thin thermal plasma model is shown with the green, black, and red solid lines. The bottom panel shows the residuals between the data and the model.
Paper: Further Evidence for the ∼9 s Pulsation in LS 5039 from NuSTAR and ASCA
Authors: Kazuo Makishima, Nagomi Uchida, Hiroki Yoneda, Teruaki Enoto, Tadayuki Takahashi
Figure caption: Pulse period of LS 5039 measured with ASCA, compared with those from Suzaku and NuSTAR. The red line connects the Suzaku and NuSTAR data points, whereas the blue one represents an average spin-down trend.
Paper: Nature of Turbulence inside Small-scale Magnetic Flux Ropes near the Sun: Parker Solar Probe Observations
Authors: Zubair I. Shaikh, Geeta Vichare, Ankush Bhaskar, Anil N. Raghav, Sofiane Bourouaine
Figure caption: Same as Figure 2 but for different SSMFRs listed in Table 1.
Paper: Nature of Turbulence inside Small-scale Magnetic Flux Ropes near the Sun: Parker Solar Probe Observations
Authors: Zubair I. Shaikh, Geeta Vichare, Ankush Bhaskar, Anil N. Raghav, Sofiane Bourouaine
Figure caption: The distribution of spectral index (same as Figure 3) for 42 SSMFRs during low-frequency (left) and high-frequency range (right).
Paper: Nature of Turbulence inside Small-scale Magnetic Flux Ropes near the Sun: Parker Solar Probe Observations
Authors: Zubair I. Shaikh, Geeta Vichare, Ankush Bhaskar, Anil N. Raghav, Sofiane Bourouaine
Figure caption: Same as Figure 3 but for the case of central 50% data points within the SSMFRs.
Paper: The Metallicity and Distance of Leo A from Blue Supergiants
Authors: Miguel A. Urbaneja, Fabio Bresolin, Rolf-Peter Kudritzki
Figure caption: The FGLR of the Leo A BSGs. The green line is the fitting relation described in the text.