adsabs/AstroCLIMB huggingface dataset:
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: Timing residuals for six of the pulsars in this analysis. The residuals at 149 MHz from LOFAR observations are plotted in orange, while the 350, 820, 1500, and 2000 MHz residuals from GBT observations are plotted in red, blue, purple, and yellow, respectively. The dashed gray lines correspond to a residual of zero. Error bars are the 1σ uncertainties at each TOA.
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: Flux density (S  ν ) measurements and best-fit power-law spectra for PSRs J0636+5128, J1327+3423, J1434+7257, and J1816+4510. The triangle in the bottom right plot represents an upper limit based on our lack of a detection of PSR J1816+4510 at 2 GHz.
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: Timing residuals for six pulsars, with the 430 and 1380 MHz residuals from NANOGrav AO observations plotted in pink and purple, respectively, and the 350 and 820 MHz residuals from GBT observations plotted in red and blue, respectively. The dashed gray lines correspond to a residual of zero. Error bars are the 1σ uncertainties at each TOA.
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: Timing residuals for the final four pulsars, with the 350 and 820 MHz residuals from GBT observations plotted in red and blue, respectively. The dashed gray lines correspond to a residual of zero. Error bars are the 1σ uncertainties at each TOA.
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: Timing residuals for five pulsars, with the 350 and 820 MHz residuals from GBT observations plotted in red and blue, respectively. The dashed gray lines correspond to a residual of zero. Error bars are the 1σ uncertainties at each TOA.
Paper: Electromagnetic Cascade Emission from Neutrino-coincident Tidal Disruption Events
Authors: Chengchao Yuan, 成超 袁, Walter Winter
Figure caption: Left column: electromagnetic cascade and neutrino spectra at the time of the neutrino observation t  ν . The black and magenta curves show the spectra of EM cascade and single-flavor neutrino emissions. The blackbody IR, OUV, and X-ray spectra are depicted as the thin cyan dotted curves. The thin blue dashed, orange dashed–dotted, green dotted, and red curves represent the components contributing to the EM cascade. The blue, red, and green shaded areas depict the energy ranges of XRT, Fermi-LAT, and HAWC observations, whereas the gray shaded areas indicate where γ γ attenuation with CMB and EBL prohibits the observation of the emitted gamma-rays. Right column: Neutrino, γ-ray, and X-ray light curves. The the magenta, green, orange, and blue solid curves illustrate the single-flavor neutrino (﹩{L}_{\nu }/4\pi {d}_{L}^{2}﹩), very high-energy (VHE) γ-ray (0.3–100 TeV), γ-ray (0.1–800 GeV), and X-ray light curves, respectively. The flux upper limits from HAWC, Fermi, and XRT/XMM/NICER or eROSITA (Cannizzaro et al. 2021; Predehl et al. 2021; Stein et al. 2021; Reusch et al. 2022) are shown as the green, orange, and blue points, respectively. Furthermore, the neutrino detection times are marked as vertical magenta dotted curves. The OUV fluxes are also plotted as gray dashed curves for reference. Light blue shaded areas and curves correspond to XRT (0.3–10 keV), whereas dark blue shaded areas and curves to eROSITA (0.3–2 keV). The upper and lower rows correspond to AT2019dsg and AT2019fdr, respectively. All panels are shown for model M-IR in the observer’s frame.
Paper: Electromagnetic Cascade Emission from Neutrino-coincident Tidal Disruption Events
Authors: Chengchao Yuan, 成超 袁, Walter Winter
Figure caption: Time-dependent evolution of IR, OUV, X-ray, and injected proton luminosities, shown as the orange, red, blue, and black solid curves, respectively. The dissipation efficiency ﹩{\varepsilon }_{\mathrm{diss}}={L}_{p}/(\dot{M}{c}^{2})\simeq 0.2﹩ is used to obtain the proton injection luminosity L  p  for AT2019dsg (left panel) and AT2019fdr (right panel). The horizontal green dashed curves represent the Eddington luminosity L Edd. The OUV luminosity peaks (t pk) and neutrino detection times (t  ν  − t pk) are illustrated as the vertical gray solid and magenta dotted curves, respectively.
Paper: Electromagnetic Cascade Emission from Neutrino-coincident Tidal Disruption Events
Authors: Chengchao Yuan, 成超 袁, Walter Winter
Figure caption: Number of expected single-flavor neutrino events as a function of R and ﹩{E}_{p,\max }﹩ as given by the color scales; we use the IceCube gamma-ray follow-up (GFU) effective areas to compute the neutrino numbers. The panels correspond to AT2019dsg (upper row) and AT2019fdr (lower row), and magnetic field strengths B = 0.1 G (left column) and 1 G (right column). The Fermi γ-ray upper limits on the ﹩R\mbox{--}{E}_{p,\max }﹩ plane are shown as red curves (the parameters in the upper left corners are excluded), and the regions where the optical thickness ﹩{\tau }_{p\gamma }^{\mathrm{fs}}({E}_{p\gamma ,\max })=1﹩ are shown as blue dashed curves (the parameters in the upper left corners are optically thick); here, the p γ optical depth is evaluated at t  ν  and ﹩{E}_{p\gamma ,\max }﹩ and the definition of ﹩{E}_{p\gamma ,\max }﹩ can be found in the main text. Moreover, the models M-X, M-IR, and M-OUV models are marked by stars.
Paper: Electromagnetic Cascade Emission from Neutrino-coincident Tidal Disruption Events
Authors: Chengchao Yuan, 成超 袁, Walter Winter
Figure caption: Electromagnetic cascade spectra and neutrino spectra at t  ν  (left column), along with neutrino, γ-ray, and X-ray light curves (right column), for the M-OUV model. The curves, areas, and data points have the same meanings as in Figure 3.
Paper: Electromagnetic Cascade Emission from Neutrino-coincident Tidal Disruption Events
Authors: Chengchao Yuan, 成超 袁, Walter Winter
Figure caption: Proton interaction rates at neutrino detection time t  ν  for AT2019dsg, as a function of proton energy (in the observer’s frame). The left and right panels correspond to the M-IR and M-OUV scenarios. In each figure, the p γ, pp with η  w  = 0.2, Bethe–Heitler (BH), escape, and dynamical rates are shown as the blue, green, orange, red, and magenta curves. The horizontal curves depict the free-streaming rate ﹩{t}_{\mathrm{fs}}^{-1}={(R/c)}^{-1}﹩, whereas the vertical gray curves show the maximum injected proton energies ﹩{E}_{p,\max }﹩.
Paper: Electromagnetic Cascade Emission from Neutrino-coincident Tidal Disruption Events
Authors: Chengchao Yuan, 成超 袁, Walter Winter
Figure caption: Comparison of EM cascade emission (black solid curve) with the leptonic contribution (dashed curves). The shaded areas have the same meanings as those in the upper left panel of Figure 3. To obtain the EM cascade spectrum, the parameters used in M-IR scenario of AT2019dsg are applied (e.g., B = 0.1 G). From the upper to lower dashed curves, the ratio of injected electron luminosity to the proton luminosity, K  e/p  ≡ L  e /L  p , varies from 1 to 10−4. The blue and orange dotted curves show the synchrotron and inverse Compton components of the L  e /L  p  = 1 case.
Paper: Electromagnetic Cascade Emission from Neutrino-coincident Tidal Disruption Events
Authors: Chengchao Yuan, 成超 袁, Walter Winter
Figure caption: Interaction rates for secondary processes, including muon decay (magenta solid), charged pion decay (green solid), γ γ attenuation (red dashed–dotted), electron/positron synchrotron (blue dashed), and inverse Compton (orange dashed) at the time of the neutrino emission. The p γ and free-streaming rates are shown as a black solid curve and a dotted horizontal line, respectively.
Paper: An Anisotropic Density Turbulence Model from the Sun to 1 au Derived from Radio Observations
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Xingyao Chen, Nicolina Chrysaphi, Francesco Azzollini, Natasha L. S. Jeffrey, Mykola Gordovskyy
Figure caption: Left: normalization coefficient ﹩{C}_{n}^{2}(r)﹩ of the density spectrum given by Equation (27), with q  i  = ω ci/(v Ti + v A) (see Figure 7). As in Figure 6, the solid/dashed lines are for anisotropy factors α = 0.25 (fundamental) and 0.42 (harmonic), respectively, and the gray region denotes the range from ﹩[1/2,2]\times \overline{q\,{\epsilon }^{2}}\,{R}_{\odot }﹩. The data from Coles & Harmon (1989) are calculated using the values of ﹩\overline{q\,{\epsilon }^{2}}\,{R}_{\odot }﹩, with q  i  inferred from the break at the larger wavenumber of their density spectrum. They gray points show where the inner scale was not well defined in their data. The data from Marsch & Tu (1990) are found via a power-law fit of the form A  q −5/3 to the density spectra in their Figure 6, where the slope corresponds to a power-law index of −5/3, and ﹩{C}_{n}^{2}(r)=A\,{n}^{2}(r)/4\pi ﹩, with n taken from Equation (A1). The dotted line shows the relation ﹩{C}_{n}^{2}(r)=3.5\times {10}^{3}\,{\left(r/{R}_{\odot }-1\right)}^{-4.7}﹩. Right: as in the left panel, but divided by n 2, with n given by Equation (A1).
Paper: An Anisotropic Density Turbulence Model from the Sun to 1 au Derived from Radio Observations
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Xingyao Chen, Nicolina Chrysaphi, Francesco Azzollini, Natasha L. S. Jeffrey, Mykola Gordovskyy
Figure caption: Observed source position vs. frequency (Shain & Higgins 1959; Wild et al. 1959; Morimoto & Kai 1961; Gurnett et al. 1978; Bougeret et al. 1984a; Reiner et al. 1998, 2009; Chrysaphi et al. 2018). The colored lines represent the observed positions from the simulations for the fundamental (left) and harmonic (right) at various values of the anisotropy parameter α and the turbulence profile ﹩\overline{q\,{\epsilon }^{2}}\,{R}_{\odot }﹩, multiplied by 1/4 (lower bound) to 4 (upper bound). The gray region shows the spread across values for an anisotropy parameter α = 0.25. The black dashed and dotted lines show the locations corresponding to the fundamental (plasma frequency) and harmonic (double plasma frequency), respectively.
Paper: An Anisotropic Density Turbulence Model from the Sun to 1 au Derived from Radio Observations
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Xingyao Chen, Nicolina Chrysaphi, Francesco Azzollini, Natasha L. S. Jeffrey, Mykola Gordovskyy
Figure caption: Top panels: simulated FWHM source sizes of Type III bursts. The simulations were performed for turbulence profiles ﹩\overline{q\,{\epsilon }^{2}}\,{R}_{\odot }﹩ given by Equation (14), multiplied by factors of [1/4,/1/2, 1, 2, 4], for values of the anisotropy parameter α = [0.19, 0.25, 0.33, 0.42], and for both fundamental (left panels) and harmonic emission (right panels). Bottom panels: average FWHM size observations (Bougeret et al. 1970; Abranin et al. 1976, 1978; Alvarez 1976; Chen & Shawhan 1978; Dulk & Suzuki 1980; Steinberg et al. 1985; Saint-Hilaire et al. 2013; Krupar et al. 2014; Kontar et al. 2017) and spikes (Clarkson et al. 2023). Simulated sizes from anisotropic scattering simulations at the fundamental (left) and harmonic (right) are overlaid with colored lines at various values of α, with turbulence levels ranging from ﹩0.5\,\overline{q\,{\epsilon }^{2}}\,{R}_{\odot }﹩ (lower) to ﹩2\,\overline{q\,{\epsilon }^{2}}\,{R}_{\odot }﹩ (upper), where the nominal ﹩\overline{q\,{\epsilon }^{2}}\,{R}_{\odot }﹩ profile is given by Equation (14). The gray region shows the spread for α = 0.25, which is consistent with the observations.
Paper: An Anisotropic Density Turbulence Model from the Sun to 1 au Derived from Radio Observations
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Xingyao Chen, Nicolina Chrysaphi, Francesco Azzollini, Natasha L. S. Jeffrey, Mykola Gordovskyy
Figure caption: Left: amplitude of the inner-scale density fluctuations ﹩\langle \delta {{n}_{i}}^{2}\rangle ﹩ calculated from Equation (29). The gray regions are the same as in Figure 6. The dotted line shows the relation ﹩\langle \delta {{n}_{i}}^{2}\rangle =2\times {10}^{7}\,{\left(r/{R}_{\odot }-1\right)}^{-3.7}﹩. The inner scale for Coles & Harmon (1989) is taken from the start of the dissipation range visible in their model spectra, and the gray points denote where the inner scale was not well observed in their data. The Marsch & Tu (1990) values are calculated using Equation (28); for their results the inner scale is not observed and instead we use the resonant distance d  r  as the measure of the inner scale. As in Figure 6, the black and red data points correspond to the assumption of fundamental and harmonic emission, respectively. Right: as in the left panel, but divided by n 2, with n(r) given by Equation (A1).
Paper: An Anisotropic Density Turbulence Model from the Sun to 1 au Derived from Radio Observations
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Xingyao Chen, Nicolina Chrysaphi, Francesco Azzollini, Natasha L. S. Jeffrey, Mykola Gordovskyy
Figure caption: Frequency spectrum of density fluctuations (fundamental is solid, harmonic is dashed line) in accordance with the density fluctuation model, using Equation (C11) with the values of ﹩\langle \delta {n}_{i}^{2}\rangle /{n}^{2}﹩ at 1 au taken from Figure 9. The gray area shows the [1/2, 2] multiplication-factor interval used in the previous figures. The in situ fluctuation data at 1 au (Celnikier et al. 1983, 1987; Kellogg & Horbury 2005; Chen et al. 2012, 2014) are shown for comparison.
Paper: An Anisotropic Density Turbulence Model from the Sun to 1 au Derived from Radio Observations
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Xingyao Chen, Nicolina Chrysaphi, Francesco Azzollini, Natasha L. S. Jeffrey, Mykola Gordovskyy
Figure caption: Left: schematic showing the coordinate system used and its relation to the solar disk and the line of sight to an extrasolar point source with separation distance r. The broadening of point sources is calculated as an integral along z in Appendix B. Right: observed FWHM major-axis source sizes of broadened point sources (Hewish 1958; Slee 1959, 1966; Högbom 1960; Gorgolewski et al. 1962; Hewish & Wyndham 1963; Harries et al. 1970; Blesing & Dennison 1972; Woo 1978; Bradford & Routledge 1980; Narayan et al. 1989; Anantharamaiah et al. 1994). The Hewish (1958) data show points where the detector baseline orientation was specified, and we take the larger of the measurements as the assumed major-axis dimension. The solid black line shows the data fit ﹩\theta =355{\left(r/{R}_{\odot }-1\right)}^{-2.15}﹩ arcseconds, and extrapolated by the dashed line. The colored lines show the simulated data for various values of the anisotropy parameter α, with the lower and upper bounds of each region respectively denoting values of ﹩\overline{q\,{\epsilon }^{2}}\,{R}_{\odot }﹩ corresponding to 0.5× and 2× the nominal values from Equation (14). Different observations are scaled to a frequency of 1.5 GHz using a frequency dependence of f −2, as expected from Equation (9); see also Equation (B5) in Appendix B.
Paper: An Anisotropic Density Turbulence Model from the Sun to 1 au Derived from Radio Observations
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Xingyao Chen, Nicolina Chrysaphi, Francesco Azzollini, Natasha L. S. Jeffrey, Mykola Gordovskyy
Figure caption: Left:  spectrum-averaged wavenumber ﹩\overline{q\,{\epsilon }^{2}}\,{R}_{\odot }﹩ as a function of heliocentric distance r, as given by Equation (14), for fundamental emission with an anisotropy factor α = 0.25 (solid), and for harmonic emission with α = 0.42 (dashed). The gray region denotes the range from ﹩[1/2,2]\times \overline{q\,{\epsilon }^{2}}\,{R}_{\odot }﹩. The data from Coles & Harmon (1989) are retrieved from the density spectrum in their Figure 4, with a density profile n(r) taken from Equation (A1). The light gray points are not well constrained due to a lack of observations at the (dominant; see Section 2) inner-scale wavenumber q  i . The in situ density fluctuation data at 1 au (Celnikier et al. 1983, 1987; Kellogg & Horbury 2005; Chen et al. 2012) are retrieved using Equation (24), with the black points corresponding to α = 0.25 (fundamental) and the red points corresponding to α = 0.42 (harmonic). The data for Celnikier et al. (1987) are taken from their Figure 7. We use the Kellogg & Horbury (2005) spectra for densities (5–6) cm−3 and (10–15) cm−3. Right: as in the left panel but multiplied by n 2, with n(r) given by Equation (A1). The dotted line shows the relation ﹩\overline{q\,{\epsilon }^{2}}\,{R}_{\odot }\,{n}^{2}(r)=6.5\times {10}^{14}\,{\left(r/{R}_{\odot }-1\right)}^{-5.17}﹩.
Paper: An Anisotropic Density Turbulence Model from the Sun to 1 au Derived from Radio Observations
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Xingyao Chen, Nicolina Chrysaphi, Francesco Azzollini, Natasha L. S. Jeffrey, Mykola Gordovskyy
Figure caption: Top panels: simulated solar radio burst 1/e decay times vs. frequency. The simulations were performed for turbulence profiles ﹩\overline{q\,{\epsilon }^{2}}\,{R}_{\odot }﹩ given by Equation (14) multiplied by factors of [1/4, 1/2, 1, 2, 4], and the values of the anisotropy parameter α = [0.19, 0.25, 0.33, 0.42], and for both fundamental (left panels) and harmonic emission (right panels). Bottom panels: observations of source decay times. The solid black points show measurements of Type III decay times (Alexander et al. 1969; Elgaroy & Lyngstad 1972; Alvarez & Haddock 1973a; Barrow & Achong 1975; Krupar et al. 2018; Reid & Kontar 2018), while open black points show spike decay times (McKim Malville et al. 1967; Barrow et al. 1994; Shevchuk et al. 2016; Clarkson et al. 2023). The solid black lines represent power-law fits to the spike data from Equation (3) of Clarkson et al. (2023) and to the Type III data from Equation (51) of Kontar et al. (2019). The light blue points show Type IIIb striae median decay times observed by PSP between 0.95 and 2.15 MHz. The colored lines represent simulated decay times from anisotropic scattering simulations at the fundamental (left panel) and harmonic (right panel). The lower and upper bound of each region denotes values corresponding to turbulence profiles of ﹩0.5\,\overline{q\,{\epsilon }^{2}}\,{R}_{\odot }﹩ and ﹩2\,\overline{q\,{\epsilon }^{2}}\,{R}_{\odot }﹩, respectively.
Paper: An Anisotropic Density Turbulence Model from the Sun to 1 au Derived from Radio Observations
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Xingyao Chen, Nicolina Chrysaphi, Francesco Azzollini, Natasha L. S. Jeffrey, Mykola Gordovskyy
Figure caption: Left: measured turbulence inner scales ﹩{q}_{i}^{-1}﹩ (Yakovlev et al. 1980; Scott et al. 1983; Coles & Harmon 1989; Manoharan 1993b; Anantharamaiah et al. 1994; Yamauchi et al. 1996, 1998), and magnetic field fluctuations (Bruno & Trenchi 2014; Chiba et al. 2022; Lotz et al. 2023), together with theoretical profiles of key plasma parameters: the proton inertial length d  i  = c/ω pi, the proton gyroradius ρ  i  = v Ti/ω ci, and the proton resonance distance d  r  = (v Ti + v A)/ω ci, calculated using the plasma and magnetic field parameters in Appendix A. The dotted curve shows the relation ﹩{q}_{i}^{-1}=2.5\times {10}^{4}\,{\left(r/{R}_{\odot }-1\right)}^{1.3}﹩ cm and the dashed line shows the inner-scale model ﹩{q}_{i}^{-1}={10}^{5}\,r/{R}_{\odot }﹩ cm by Coles & Harmon (1989). Right: the same as the left panel, but for the inner-scale wavenumber q  i .
Paper: An Anisotropic Density Turbulence Model from the Sun to 1 au Derived from Radio Observations
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Xingyao Chen, Nicolina Chrysaphi, Francesco Azzollini, Natasha L. S. Jeffrey, Mykola Gordovskyy
Figure caption: Left panel: coronal density model (black solid line) given by Equation (A1). Other coronal density models (Allen 1947; Newkirk 1961; Alvarez & Haddock 1973b; Saito et al. 1977; Bougeret et al. 1984b; Bird et al. 1994; Leblanc et al. 1998; Mancuso & Spangler 2000) are also shown, within the ranges of their respective validity. The models from Bird et al. (1994) and Mancuso & Spangler (2000) are as used in Spangler (2002). Right panel: magnetic field model (black solid line) given by Equation (A2), together with observations (Burlaga & Ness 1968; Villante & Mariani 1975; Behannon 1976; Dulk & McLean 1978; Rosenberg et al. 1978; Patzold et al. 1987; Sakurai & Spangler 1994; Lin et al. 2000; Spangler 2005, 2020; Ramesh et al. 2010; Gopalswamy et al. 2012; Kolotkov et al. 2018). The red line shows the model of Dulk & McLean (1978).
Paper: Discovery and Timing of Millisecond Pulsars with the Arecibo 327 MHz Drift-scan Survey
Authors: Evan F. Lewis, Timothy E. E. Olszanski, Julia S. Deneva, Paulo C. C. Freire, Maura A. McLaughlin, Kevin Stovall, Manjari Bagchi, Jose G. Martinez, Benetge B. P. Perera
Figure caption: Polarization-calibrated composite profiles for PSRs J1630+3550 (top) and J2055+1545 (bottom), with polarization position angle. The pulse profile for J1630 is centered at a pulse phase of 0.5, with the best-fit RM of 8.72 rad m−2 applied. The main component of the profile for J2055 is centered at a pulse phase of 0.25, with the interpulse visible at a phase of 0.75. For J2055, the best-fit RM of –65.3 rad m−2 has been applied. The y-axes are in arbitrary units. Black lines represent total intensity (Stokes I ), red lines represent linear polarization (Stokes L), and blue lines represent circular polarization (Stokes V ).
Paper: An Anisotropic Density Turbulence Model from the Sun to 1 au Derived from Radio Observations
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Xingyao Chen, Nicolina Chrysaphi, Francesco Azzollini, Natasha L. S. Jeffrey, Mykola Gordovskyy
Figure caption: Forms of the parallel and perpendicular wavenumber spectra corresponding to the two cases described in Appendices C.2 (Equation (C9); left) and C.3 (Equation (C13); right). In the former case, the spectral break points are different for the parallel and perpendicular directions, while in the latter case the spectral break points for both directions are the same. In both plots, both axes are on logarithmic scales.