adsabs/AstroCLIMB huggingface dataset:
Paper: Vibrational Spectroscopy of ﹩{{\rm{C}}}_{60}^{+}﹩ and ﹩{{\rm{C}}}_{70}^{+}﹩ in the Mid-infrared: A Comparison with Astronomical Observations
Authors: Thomas E. Douglas-Walker, Olivia O'Neill, Ewen K. Campbell
Figure caption: Photofragmentation spectrum of ﹩{{\rm{C}}}_{70}^{+}-{\rm{He}}﹩ (black) and ﹩{{\rm{C}}}_{70}^{+}-{{\rm{He}}}_{2}﹩ (red). ﹩{{\rm{C}}}_{70}^{+}-{{\rm{He}}}_{2}﹩ spectrum is offset vertically for clarity and shows a redshift of less than 1 cm−1 compared to ﹩{{\rm{C}}}_{70}^{+}-{\rm{He}}﹩.
Paper: Vibrational Spectroscopy of ﹩{{\rm{C}}}_{60}^{+}﹩ and ﹩{{\rm{C}}}_{70}^{+}﹩ in the Mid-infrared: A Comparison with Astronomical Observations
Authors: Thomas E. Douglas-Walker, Olivia O'Neill, Ewen K. Campbell
Figure caption: Mass spectrum of ﹩{{\rm{C}}}_{60}^{+}﹩ following storage in dense helium buffer gas at 4.7 K.
Paper: Starspot Temperature of CoRoT-2 from Multiwavelength Observations with SPARC4
Authors: Adriana Valio, Eder Martioli, Andre O. Kovacs, Viktor Y. D. Sumida, Leandro de Almeida, Diego Lorenzo-Oliveira, Francisco Jablonski, Claudia V. Rodrigues
Figure caption: Light curves of the transit of CoRoT-2 b in the four photometric bands of SPARC4, with the smoothed data shown in green and a model of a spotless star depicted in blue. The bottom panels of each wave band show the residuals, after subtraction of a spotless star model (blue curve in the top panel). The time at transit center is 2460507.10 BJD. The red curves show the result of the model fitting for two spots. The horizontal dashed lines represent a 2σ threshold for the signal to be considered due to a spot (1σ = 930, 530, 580,  and 570 ppm for the smoothed signal from bands g, r, i, and z, respectively).
Paper: Starspot Temperature of CoRoT-2 from Multiwavelength Observations with SPARC4
Authors: Adriana Valio, Eder Martioli, Andre O. Kovacs, Viktor Y. D. Sumida, Leandro de Almeida, Diego Lorenzo-Oliveira, Francisco Jablonski, Claudia V. Rodrigues
Figure caption: Starspot temperature estimation using blackbody fitting. The red and orange dots represent the observed spot intensities in the four photometric bands (g, r, i, and z), whereas the red and orange curves correspond to the best-fit blackbody spectra, yielding temperatures of 5110  ±  140 K for spot 1 (longitude of 20°) and 5040  ±  190 K for spot 2 (longitude of −50°). The stellar photosphere is assumed to have an effective temperature of 5529 K (green curve).
Paper: Starspot Temperature of CoRoT-2 from Multiwavelength Observations with SPARC4
Authors: Adriana Valio, Eder Martioli, Andre O. Kovacs, Viktor Y. D. Sumida, Leandro de Almeida, Diego Lorenzo-Oliveira, Francisco Jablonski, Claudia V. Rodrigues
Figure caption: Starspot temperature estimation using PHOENIX stellar atmosphere models. The blue curve shows the PHOENIX spectrum for a 5529 K star (log(g) = 4.48, [Fe/H] = −0.04, [α/M] = 0.0). The red dots represent the observed spot intensities in the four photometric bands (g, r, i, and z). The red and orange curves correspond to the best-fit PHOENIX spectra, yielding temperatures of 5130  ±  120 K for spot 1 (longitude of 20°) and 5060  ±  200 K for spot 2 (longitude of −50°).
Paper: Vibrational Spectroscopy of ﹩{{\rm{C}}}_{60}^{+}﹩ and ﹩{{\rm{C}}}_{70}^{+}﹩ in the Mid-infrared: A Comparison with Astronomical Observations
Authors: Thomas E. Douglas-Walker, Olivia O'Neill, Ewen K. Campbell
Figure caption: Comparison of calculated IR spectra of ﹩{{\rm{C}}}_{70}^{+}﹩ in Cs (red) and C2v (blue) symmetries using the B3LYP/6-311G* functional and basis set. The stick spectra are convolved with Lorentzian functions with an FWHM of 10 cm−1.
Paper: Starspot Temperature of CoRoT-2 from Multiwavelength Observations with SPARC4
Authors: Adriana Valio, Eder Martioli, Andre O. Kovacs, Viktor Y. D. Sumida, Leandro de Almeida, Diego Lorenzo-Oliveira, Francisco Jablonski, Claudia V. Rodrigues
Figure caption: MCMC results of the simultaneous multiwavelength fitting for spot temperature estimation. The best-fit models for both spots assume a single temperature, longitude, and radius across all four photometric bands. The left panel shows the fit for the spot at longitude 20°, while the right panel shows the fit for the spot at longitude −50°.
Paper: Starspot Temperature of CoRoT-2 from Multiwavelength Observations with SPARC4
Authors: Adriana Valio, Eder Martioli, Andre O. Kovacs, Viktor Y. D. Sumida, Leandro de Almeida, Diego Lorenzo-Oliveira, Francisco Jablonski, Claudia V. Rodrigues
Figure caption: Results of the MCMC fit to spot at longitude 20° in the residuals of the transit light curve for the four photometric bands. The fit parameters of the spot are radius (in units of planetary radius), intensity, and longitude. The plots show the MCMC samples and the respective posterior distributions of each free parameter.
Paper: Vibrational Spectroscopy of ﹩{{\rm{C}}}_{60}^{+}﹩ and ﹩{{\rm{C}}}_{70}^{+}﹩ in the Mid-infrared: A Comparison with Astronomical Observations
Authors: Thomas E. Douglas-Walker, Olivia O'Neill, Ewen K. Campbell
Figure caption: Mass spectrum of ﹩{{\rm{C}}}_{70}^{+}﹩ following storage in dense helium buffer gas at 4.7 K.
Paper: Starspot Temperature of CoRoT-2 from Multiwavelength Observations with SPARC4
Authors: Adriana Valio, Eder Martioli, Andre O. Kovacs, Viktor Y. D. Sumida, Leandro de Almeida, Diego Lorenzo-Oliveira, Francisco Jablonski, Claudia V. Rodrigues
Figure caption: Same as Figure 4 for the second spot at longitude −50°.
Paper: Development of Turbulence in Postshock Regions
Authors: Michael M. Foley, Philip Mocz, Blakesley Burkhart, Lars Hernquist, Alyssa Goodman
Figure caption: Top: projection of the density for a snapshot of the M15_T2_decay run. Different lines indicate different slices taken through the simulation domain where the curl and divergence are calculated. Starting at the right, the first black line indicates preshock gas. The second black line indicates the approximate region of the start of the shock. The red line indicates the shock density peak. The third black line indicates the scale height of the postshock region. Finally, the fourth black line shows the end of the postshock region. Top slices: density at each slice in the simulation domain. Density is given in code units, which can be scaled to physical units using the scalings introduced earlier in the paper. Middle slices: divergence of the velocity field at each slice in the simulation domain. Negative values for the divergence indicate compressive motions, while positive values indicate diffusive ones. Bottom slices: curl of the velocity field at each slice in the simulation domain. Larger values indicate stronger vorticity, while smaller values indicate more laminar flow.
Paper: Development of Turbulence in Postshock Regions
Authors: Michael M. Foley, Philip Mocz, Blakesley Burkhart, Lars Hernquist, Alyssa Goodman
Figure caption: Left: 3D kinetic energy power spectrum of the preshock and postshock regions for a Mach 15 shock passing through either Mach 2 or Mach 5 driven turbulence. L is the characteristic length of the box. The power spectra are divided by k−2 to aid visualization. The gray region roughly indicates the inertial range of the spectra where the slopes should be evaluated. All spectra appear to follow a Burgers scaling of k−2. Right: 3D kinetic energy power spectrum of three different time snapshots for a Mach 15 shock passing through Mach 2 decaying turbulence. At early times, the shock appears to follow a k−2 scaling but decays to k−5/3 more quickly than the surrounding turbulence.
Paper: Development of Turbulence in Postshock Regions
Authors: Michael M. Foley, Philip Mocz, Blakesley Burkhart, Lars Hernquist, Alyssa Goodman
Figure caption: Top: mass projection of a shock with ﹩{{ \mathcal M }}_{s}=15﹩ and Mt = 2 after one shock crossing time (where a crossing time is defined as ﹩{t}_{{\rm{cross}}}={L}_{{\rm{box}}}/{{ \mathcal M }}_{s,{\rm{initial}}}﹩) for a 512 × 128 × 128 run. The low-density region on the left of the plot is the rarefaction wave, and the shock is traveling to the right. Middle: projection of energy dissipated by turbulence for the same snapshot. Dissipation is observed to be the strongest in the dense regions, though it does not perfectly track density. Bottom: projection of kinetic energy for the same snapshot. As the shock propagates, it develops protrusions of high kinetic energy surrounded by regions of kinetic energy closer to the ambient turbulence.
Paper: Development of Turbulence in Postshock Regions
Authors: Michael M. Foley, Philip Mocz, Blakesley Burkhart, Lars Hernquist, Alyssa Goodman
Figure caption: Log density and energy profiles for a single snapshot of the M15_2_decay run. The density profile is shown in blue, the total turbulent energy is shown in red, the turbulent energy in the y- and z-directions (fluctuations parallel to the shock front) is shown in green, and the turbulent energy in x (fluctuations in the direction of shock propagation) is shown in yellow. Each profile is expressed as the ratio of the value at a given box index to the median value across the whole preshock.
Paper: Development of Turbulence in Postshock Regions
Authors: Michael M. Foley, Philip Mocz, Blakesley Burkhart, Lars Hernquist, Alyssa Goodman
Figure caption: Top: mass projection of the turbulent conditions for the 512 × 128 × 128 resolution runs with Mach 2 turbulence after five crossing times. At this snapshot, a velocity pulse is injected to produce a shock. Middle: projection of energy dissipated throughout turbulence in the simulation box for the same snapshot. Dissipation is the strongest in the densest regions, though the dissipation does not perfectly track density. Bottom: kinetic energy in the box at the moment of shock injection. A Gaussian velocity pulse is injected at the left of the box. Turbulence remains in the rest of the box, and kinetic energy generally matches the mass distribution.
Paper: Development of Turbulence in Postshock Regions
Authors: Michael M. Foley, Philip Mocz, Blakesley Burkhart, Lars Hernquist, Alyssa Goodman
Figure caption: Density projections of shocks moving into both decaying and driven turbulence at 1024 × 256 × 256 resolution. Increasing shock Mach number ﹩{{ \mathcal M }}_{\mathrm{Shock}}﹩ is shown from left to right, and all simulations are run with ﹩{{ \mathcal M }}_{t}=2﹩. All snapshots are taken when the shock front/remaining density enhancement reaches a location of 0.5 in code units with the shock propagating to the right. Comparing the 1024 × 256 × 256 panels to Figure 1 shows that resolution does not appear to have a major effect on the topology of the shock, at least at early times.
Paper: Development of Turbulence in Postshock Regions
Authors: Michael M. Foley, Philip Mocz, Blakesley Burkhart, Lars Hernquist, Alyssa Goodman
Figure caption: Top: projection of the divergence of the 3D velocity field for a snapshot of the M15_T2_decay run. The solid black line indicates the shock density peak, the left black dashed line indicates the scale height of the postshock region, and the right black dashed line indicates the transition point from preshock to shock. Red regions are compressing, and blue regions are dispersing. Bottom: projection of curl of the velocity field. As in the top plot, the black lines correspond to the shock region boundaries. Blue regions possess strong vorticity, while red regions are characterized by flow with little rotation.
Paper: Development of Turbulence in Postshock Regions
Authors: Michael M. Foley, Philip Mocz, Blakesley Burkhart, Lars Hernquist, Alyssa Goodman
Figure caption: Density projections of shocks moving into either driven turbulence (purple outline) or decaying turbulence (blue outline) at 512 × 128 × 128 resolution. Increasing shock Mach number ﹩{{ \mathcal M }}_{s}﹩ is shown from left to right, and increasing turbulent Mach number ﹩{{ \mathcal M }}_{t}﹩ is shown from bottom to top. All snapshots are taken when the shock front/remaining density enhancement reaches a location of 0.5 in code units while propagating to the right. Shocks moving into decaying turbulence generally maintain a more coherent structure for longer.
Paper: Development of Turbulence in Postshock Regions
Authors: Michael M. Foley, Philip Mocz, Blakesley Burkhart, Lars Hernquist, Alyssa Goodman
Figure caption: Top: projection of turbulent dissipation for the same snapshot as shown in Figure 5. Lines overlaid show the slices over which the histogram of oriented gradients (HOG) was computed in the postshock region. The black vector indicates the shock normal vector. Middle: HOG for the vorticity field. For every slice in the top plot, the angle between the vorticity vector and the shock normal is calculated. Counts of each angle are binned, tallied, and reported as a histogram for each region. Counts are normalized to the mean preshock value, which is divided out to highlight deviations. Bottom: schematic showing the different vorticity orientations that are enhanced or depressed in the HOG. Low angles between ω and ﹩{\boldsymbol{n}}﹩ correspond to streamwise vorticity and high angles correspond to transverse vorticity.
Paper: Development of Turbulence in Postshock Regions
Authors: Michael M. Foley, Philip Mocz, Blakesley Burkhart, Lars Hernquist, Alyssa Goodman
Figure caption: Top left: mass column density for the shock region in a snapshot of the M15_T2_decay run. The dotted lines indicate the bounds of the shock front and postshock regions, and the solid black line indicates the shock peak. Top right: projection of negative divergence (convergence) of the velocity field in units of column density per megayear (M⊙ Myr–1 Pc–2). Bottom right: projection of positive divergence of the velocity field in the same units as above. Bottom left: a composite of the top-right and bottom-right plots, with projections of positive divergence and negative divergence overlaid. Converging regions are indicated in red, and diverging regions are indicated in blue. The range of the mass flow is the same for both converging and diverging motions.
Paper: Development of Turbulence in Postshock Regions
Authors: Michael M. Foley, Philip Mocz, Blakesley Burkhart, Lars Hernquist, Alyssa Goodman
Figure caption: Left: streamwise and transverse vorticity enhancement in the shock region for runs with decaying ﹩{{ \mathcal M }}_{t}=2﹩ turbulence. The y-axis is shown as a log scale with reference values provided. Solid lines indicate transverse vorticity measured at the shock front, and dotted lines indicate streamwise vorticity measured at the end of the postshock region. Different colors indicate different runs where the shock Mach number ﹩{{ \mathcal M }}_{s}﹩ is varied. Right: same as left panel but for simulation runs with driven ﹩{{ \mathcal M }}_{t}=2﹩ turbulence.
Paper: Electron Acceleration in Thinning Nonreconnecting Current Sheets in a Quasi-parallel Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: Time evolution of Jz in a local region that contains an ion-scale (di-scale) magnetic island and a few reconnection X-lines. The black curves are magnetic field lines. The yellow “X” mark is an X-line where ion-coupled reconnection occurs. The white arrow is the current sheet that is thinning. The white and magenta X-lines exist in the bottom part of the thinning current sheet.
Paper: Electron Acceleration in Thinning Nonreconnecting Current Sheets in a Quasi-parallel Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: (a) Current density Jz at Ωit = 20.0. (b) Electron temperature Te. The black curves are magnetic field lines. The shock plane is at x = 45di, and the shock is propagating in the positive x-direction. Near the shock plane, magnetic field lines are bent and many current sheets are produced.
Paper: Electron Acceleration in Thinning Nonreconnecting Current Sheets in a Quasi-parallel Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: (a)–(c) Magnetic field lines (black) and an electron trajectory in a thinning current sheet with Jz < 0 (red). The yellow and blue dots are the start and end times for each time interval. (d) The time evolution of the Lorentz factor γ (red) and the theoretical curves based on Equation (12). The green and blue curves are for f(θ0) = 1 and 0.8. (e) Work done by the electric field. Wx (red), Wy (blue), and Wz (green) are for the work done by the x-, y-, and z-components of the electric field. Wtotal (black) is the sum of Wx, Wy, and Wz. W∥ (magenta) is the work done by the parallel electric field. (f) The perpendicular momentum p⊥ (red), the parallel momentum p∥ (blue), and the magnetic moment (green).
Paper: Electron Acceleration in Thinning Nonreconnecting Current Sheets in a Quasi-parallel Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: (a) Schematic of the trajectory of an electron (thick curve) in a current sheet with Jy < 0. The angle θ0 is the angle between the solid line and the vertical dashed line. The dashed trajectory outside the shaded region is the one between the exit position (at t = (π + 2θ0)/Ωc) and the next entrance position (t = 0). (b) Schematic of the trajectory of a meandering electron in a current sheet with Jz > 0. The particle moves in a range of angle 2θ0 in the blue shaded region, exits the current sheet, and reenters the current sheet (blue shaded region), moving with 2θ0 again. The trajectory in the pink shaded region is symmetric to the one in the blue shaded region.
Paper: Electron Acceleration in Thinning Nonreconnecting Current Sheets in a Quasi-parallel Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: Schematic of a thinning current sheet with Jz < 0. (a) Magnetic field (black) in the x–y plane. The shaded region has Bz < 0, moving with a speed Vc toward the left. As a result, the motional electric field (blue) is produced. (b) A simplified thinning current sheet and an electron trajectory whose guiding center is moving downward (red). (c) The trajectory of an electron whose guiding center is moving upward (red).
Paper: Electron Acceleration in Thinning Nonreconnecting Current Sheets in a Quasi-parallel Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: Schematic of a thinning current sheet with Jz > 0. (a) Magnetic field (black) in the x–y plane. The pink and blue shaded regions have By = −Bc and By = Bc, respectively, moving with a speed Vc/2 toward the center. As a result, the motional electric field Ez (green) is produced in the positive z-direction in both regions. The electron is meandering in the current sheet (red). (b) The same current sheet in the x–z plane. The motional electric field (green) is pointing in the positive z-direction, and the meandering electron is moving in the negative z-direction (red). (c) The x–z trajectory of the electron shown in Figure 8.
Paper: Electron Acceleration in Thinning Nonreconnecting Current Sheets in a Quasi-parallel Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: The trajectory and energization history for another electron that is accelerated in a thinning current sheet with Jz > 0. The same format as Figure 7. In panel (d), the green and blue curves are based on Equation (18) for g(θ0)/f(θ0) = 1 and 0.6, respectively.
Paper: Electron Acceleration in Thinning Nonreconnecting Current Sheets in a Quasi-parallel Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: Field quantities around the nonreconnecting current sheet (indicated by the white arrow in Figure 2) at Ωit = 20.0. (a) Current density Jz. (b) current density Jy. (c) Electric field Ex. (d) Electric field Ey. (e) Magnetic field Bz. (f) Electron fluid velocity Vey. In (c), (d), and (f), the white arrows show the vectors for each quantity.
Paper: Electron Acceleration in Thinning Nonreconnecting Current Sheets in a Quasi-parallel Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: (a) Electric field Ey (color) and magnetic field lines (black). The oval marks show the positions of the nonreconnecting current sheets. The white oval is the nonreconnecting current sheet shown in Figure 5. (b) Positions of energetic electrons whose Lorentz factor γ > 6 (red dots) and γ > 7.5 (blue dots). The background color is the same as in panel (a).
Paper: Electron Acceleration in Thinning Nonreconnecting Current Sheets in a Quasi-parallel Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: Time evolution of electric field Ey. The same format as Figure 2.
Paper: Electron Acceleration in Thinning Nonreconnecting Current Sheets in a Quasi-parallel Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: Time evolution of electric field Ex. The same format as Figure 2.
Paper: Rotational Spectroscopy and Tentative Interstellar Detection of 3-hydroxypropanal (HOCH2CH2CHO) in the G+0.693-0.027 Molecular Cloud
Authors: Zachary T. P. Fried, Roman A. Motiyenko, Miguel Sanz-Novo, Lucie Kolesniková, Jean-Claude Guillemin, Laurent Margulès, Tereza Uhlíková, Arnaud Belloche, Jes K. Jørgensen, Martin S. Holdren, Ci Xue, Štěpán Urban, Izaskun Jiménez-Serra, Victor M. Rivilla, Brett A. McGuire
Figure caption: Section of the room-temperature millimeter wave spectrum of 3-hydroxypropanal. Dominating lines correspond to degenerate pairs of the ground state (G.S.) a-type and b-type R-branch transitions with low Ka values of Conformer 1. The leading transition is J = 40 ← 39, and the value of J decreases by 1 with each successive line. The same pattern is observable for the v27 = 1 and v26 = 1 excited vibrational states.
Paper: Rotational Spectroscopy and Tentative Interstellar Detection of 3-hydroxypropanal (HOCH2CH2CHO) in the G+0.693-0.027 Molecular Cloud
Authors: Zachary T. P. Fried, Roman A. Motiyenko, Miguel Sanz-Novo, Lucie Kolesniková, Jean-Claude Guillemin, Laurent Margulès, Tereza Uhlíková, Arnaud Belloche, Jes K. Jørgensen, Martin S. Holdren, Ci Xue, Štěpán Urban, Izaskun Jiménez-Serra, Victor M. Rivilla, Brett A. McGuire
Figure caption: Tentative detection of 3-hydroxypropanal toward G+0.693. The selected transitions are sorted by increasing frequency and listed in Table 3. The result of the LTE model of 3-hydroxypropanal is plotted with a red line, while the blue line represents the combined emission of all molecules identified in the survey, including also 3-hydroxypropanal (observed spectra shown as gray lines and light gray-shaded histograms).
Paper: Rotational Spectroscopy and Tentative Interstellar Detection of 3-hydroxypropanal (HOCH2CH2CHO) in the G+0.693-0.027 Molecular Cloud
Authors: Zachary T. P. Fried, Roman A. Motiyenko, Miguel Sanz-Novo, Lucie Kolesniková, Jean-Claude Guillemin, Laurent Margulès, Tereza Uhlíková, Arnaud Belloche, Jes K. Jørgensen, Martin S. Holdren, Ci Xue, Štěpán Urban, Izaskun Jiménez-Serra, Victor M. Rivilla, Brett A. McGuire
Figure caption: Selection of rotational transitions of 3-hydroxypropanal, v=0 covered by the ReMoCA survey. The LTE synthetic spectrum of 3-hydroxypropanal, v=0 used to derive the upper limit to its column density toward Sgr B2(N1S) is displayed in red and overlaid on the observed spectrum shown in black. The blue synthetic spectrum contains the contributions of all molecules identified in our survey so far. The values written below each panel correspond from left to right to the HPBW, the central frequency in MHz, the width in MHz of each panel in parentheses, and the continuum level in K of the baseline-subtracted spectra in brackets. The y-axis is labeled in brightness temperature units (K). The dotted line indicates the 3σ noise level.