adsabs/AstroCLIMB huggingface dataset:
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: Velocity-coherent filaments in Orion B identified with the FoF algorithm. (a) Morphologies of the filaments. The filament names are labeled with the same colors as each filament. (b) The distribution of velocity centroids ranges from 7.8–11.5 km s−1 within identified filaments. (c) The spines of each filament are drawn with thick lines. (d) The distribution of YSOs identified and classified in Furlan et al. (2016). Red asterisk symbol: Class 0 protostars. Green asterisk symbol: Class I protostars. Yellow asterisk symbol: flat-spectrum YSOs. The colored contours delineate the filaments identified in this study. Gray tones in the two lower panels indicate the distribution of the integrated intensity of C18O (1–0) line.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: Procedures identifying velocity-coherent filamentary structures with the FoF algorithm in the Orion B region. The colored regions denote the filamentary structures identified from FoF with the criteria for spatial separation (﹩\sqrt{2}﹩ pixel size) and velocity difference  V  diff (from 0.1–0.045 km s−1) written on the bottom of the panels. The gray region in each panel is a continuously connected structure within the velocity criteria and the shades (darker regions) in the gray region indicate that there are multiple velocity components in the line of sight in the velocity-coherent structure. The insets in the panels denote C18O (1–0) spectra and their decomposed Gaussian components at a pixel point. The numbers in the insets indicate the velocity centroids of the Gaussian components at the start point of the arrow. The colors of the velocity centroid numbers and Gaussian-fit profiles correspond to the colors of the filamentary structures.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: The color scale presents a Herschel 250 μm continuum image of the Orion B region. Contours are from the integrated intensity maps of 13CO (middle left panel) and C18O (middle right panel). The contour levels for the 13CO integrated intensity map are [1, 3, 5, 7, 9, 11] K km s−1 and those for the C18O integrated intensity map are [0.25, 0.75, 1, 1.5, 2.2, 3.5, 6] K km s−1. Panels (a)–(f) show representative spectra of 13CO (black line) and C18O (blue line) at the central positions marked with green dots in the middle left panel and the middle right panel. In panel (a)–(f), the C18O spectrum is scaled up by a factor of 2 and shifted by –1 in intensity. The gray and cyan horizontal lines represent baselines of the 13CO and C18O spectra, respectively.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: Left panel: integrated intensity map of the C18O (1–0) line of Orion B. The green dot denotes the position of the central pixel of the 3 × 3 spectra in the right panel. Right panel: representative spectra are shown with results from the step-by-step decomposing procedure described in Section 3.1.1. Black solid line: original spectrum at each pixel. Blue solid line: smoothed profile with the initial smoothing parameters (Step 1). Red vertical line: initial guesses of velocity component found in Step 1. Green solid line: decomposed Gaussian profiles determined in Step 3 with modified initial guesses from Step 2. Red thick solid line: the profiles combined by decomposed Gaussian components. Red and blue horizontal dotted lines: 3σ levels of original and smoothed profiles, respectively.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: The velocity channel maps of C18O (1–0) emission in relation to the identified filamentary structures. The velocity ranges of integration are indicated in the bottom of each panel. The filament spines covering the velocity channel range of each panel are overlaid with the same colors as the ones for the filaments in Figure 7.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: The oscillatory features of the C18O (1–0) velocity centroids of the filaments along the R.A. (upper panel) and decl. (lower panel) directions. The colors of the dots are identical to the colors of the filaments in the upper-left panel of Figure 7.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: The velocity distribution of C18O (1–0) Gaussian-fit components decomposed by the Gaussian decomposition process (see Section 3.1.1).
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: The averaged J = 1–0 line profiles of 13CO (blue) and C18O (orange) throughout the whole line emitting region. Gray lines indicate the best-fit Gaussian profiles.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: Left panel: the distribution of the YSOs and the dense cores in the C18O (1–0) filament F23. The color tone indicates the image of the C18O (1–0) integrated intensity. The contours indicate the integrated intensity levels of N2H+ (1–0) [0.08, 0.3, 0.8, 2.0, 4.0, 6.0, 8.0, 10.0] K km s−1 in. The blue and green polygons display the dense cores seemingly associated with the filament in LSR velocities and the dense cores not associated with the filament, respectively. The asterisks indicate YSOs classified in Furlan et al. (2016). Red: Class 0 protostars. Green: Class I protostars. Orange: flat-spectrum YSOs. Right-upper panel: the variation of the integrated intensity along the filament spine. The red line displays the averaged intensity variation. Right-middle panel: The variation of the velocity centroids along the filament spine from C18O (1–0) (green dots) and the dense cores from N2H+ (1–0) (blue dots) associated with the filament. Right-lower panel: the variation of the nonthermal velocity dispersion divided by the speed of sound along the spine of the filament. The orange and blue dots are estimated from C18O (1–0) (for filaments) and N2H+ (1–0) (for dense cores), respectively. The vertical dashed lines are representative positions of the dense cores embedded in the filament (the blue polygons in the left panel). Red horizontal lines indicate the locations for the Mach numbers (=σ nth/c s) of 1 and 2. The inset shows histograms of the Mach number distributions of filaments and cores with the same colors as the ones in the main plots.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: The distributions of SO and NH2D in N2H+ dense cores. The integrated intensities of SO (32–21) and ortho-NH2D (111–101) are shown in magenta color tones and black contours with levels of 0.031 K km s−1 × [3, 5, 8, 11, 14, 17]), respectively. N2H+ dense cores are drawn in blue or green depending on whether NH2D is detected or not detected. Small gray shaded areas indicate the ortho-NH2D (111–101) observed regions. The YSOs from Furlan et al. (2016) are shown with asterisk symbols (red for Class 0 protostars, green for Class I protostars, and orange for flat-spectrum YSOs). Core names are labeled only for NH2D detected dense cores. Boxes drawn with dashed lines with labels (a)–(d) are the regions of close-up views in Figure 26.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: Zoom-in distribution of SO and NH2D in Orion B. The integrated intensities of ortho-NH2D (111–101) and SO (32–21) lines are shown in black and red contours, respectively. The background color tones represent the H2 column density distribution (Arzoumanian et al. 2019; Könyves et al. 2020). The contour levels for NH2D data are 0.031 K km s−1 × [2, 5, 8, 11, 14, 17] and those for SO data are 0.036 K km s−1 × [15, 22, 30, 40, 50, 65, 80, 95]. The H2 column density level in the background is indicated in the color bar. The YSOs from Furlan et al. (2016) are shown with asterisk symbols (red for Class 0 protostars, green for Class I protostars, and orange for flat-spectrum YSOs). Black circles denote the Herschel robust prestellar cores presented in Könyves et al. (2020).
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: Averaged integrated intensities of three molecular lines (N2H+, SO, and NH2D) for dense cores as a function of H2 column density measured with TRAO beam size at the N2H+ emission peak position. Blue stars and filled red and open red circles indicate gravitationally bound dense cores with YSOs, prestellar cores, and gravitationally unbound starless dense cores, respectively. Dense cores with (blue) and without (red) YSOs, where NH2D emission is undetected in our sensitivity, are marked with arrows as the upper limit (rms level at NH2D integrated intensity map).
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: The systemic velocities of dense cores measured by N2H+ (1–0) spectra in comparison with those of surrounding filaments obtained by C18O (1–0) spectra. Green and blue dots represent dense cores with and without YSOs. Red bars indicate 1σ error bars for both data sets. A solid line indicates the result for the least-squares fit for the data and dashed lines show the range from the fit result by the speed of sound of 0.23 km s−1, at the average dust temperature of 14.8 K.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: Infall asymmetries appeared in the HCO+ (1–0) (white) and H13CO+ (1–0) (cyan) line profiles toward C18 (central 3 × 3 spectra in left panel) and C28 (central 3 × 3 spectra in right panel). The color tones in the background indicate the N2H+ (1–0) integrated intensity. The dashed blue vertical line at the center indicates the systemic velocity measured from the hyperfine fitting of N2H+ (1–0). Each spectrum is the average of the spectra for the 2 × 2 pixels shown in the background of each spectrum. H13CO+ (1–0) is shown with an offset of −0.5 K in the y-axis.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: Infall asymmetries shown HCO+ (1–0) (black) and C18O (1–0) (blue) line profiles at the region of H1 marked in Figure 21. Each line profile is the average of the spectra for the 2 × 2 pixels shown in the background of each spectrum. The background color scale indicates the C18O (1–0) integrated intensity. The baselines of HCO+ (1–0) and C18O (1–0) are set to be zero and −0.5 K, respectively.
Paper: TRAO Survey of Nearby Filamentary Molecular Clouds, the Universal Nursery of Stars (TRAO-FUNS). III. Filaments and Dense Cores in the NGC 2068 and NGC 2071 Regions of Orion B
Authors: Hyunju Yoo, Chang Won Lee, Eun Jung Chung, Shinyoung Kim, Mario Tafalla, Paola Caselli, Philip C. Myers, Kyoung Hee Kim, Tie Liu, Woojin Kwon, Archana Soam, Jongsoo Kim
Figure caption: The histogram of core-to-core separations in the filament F23 using offset positions of identified N2H+ dense cores and less dense, but possible core-forming regions in the future. The vertical line indicates the median value of the separation (0.39 pc).
Paper: Theory of Magnetic Switchbacks Fully Supported by Parker Solar Probe Observations
Authors: Gabor Toth, Marco Velli, Bart van der Holst
Figure caption: Illustration of how switchbacks form. The top part of each panel shows the evolution of three magnetic field lines (solid black curves with arrows) projected to the r–y plane. The dashed lines follow r = 3π + sy, indicating the amount of shear s = 1.5t that grows linearly with time t. At time t = 0, the original circularly polarized Alfvén wave is shown with wavelength λ  r  = 2π and width w = (B ⊥/B  r )λ  r /π = 0.8 At this time, B  r  is uniform, and the magnitude of the perpendicular field is B ⊥ = 0.4B  r . The wave velocity v = 1.5y shown by the red arrows changes linearly with y. At time t = 1, the field lines are mildly distorted. By time t = 2, the field line folds over and B  r  changes sign, creating a switchback around the positions where the dashed line intersects the field lines. At t = 3, there is a substantial radial field reversal. The bottom part of each panel shows B  r (t) = B  r (t = 0) + sB  y  (solid lines) and the magnetic pressure ﹩{p}_{B}=({B}_{\perp }^{2}+{B}_{r}^{2})/(2{\mu }_{0})﹩ (dashed lines) at the four time instances. Switchbacks occur when the line enters the blue regions. The gray arrows show the gradient of the magnetic pressure that compresses the plasma and magnetic field. The red lines show numerical simulation results for comparable conditions. The switchbacks are narrow peaks between flatter background field regions. The sketch at the bottom of the figure depicts the evolution of shear in a radial outflow. The two streamlines are separated by an angle d α, and the wave velocities are v and v + dv, respectively. The dotted and solid curves show the field line without and with shear, respectively. The shear s grows fast near the starting point from s 0 = 0 to s 1 and s 2, but it eventually reaches an asymptotic maximum value of (1/v)(dv/d α). Still, due to B ⊥/B  r  ∝ r, switchbacks can form at larger radii, as shown by the radially inward-pointing black arrow on the right.
Paper: Theory of Magnetic Switchbacks Fully Supported by Parker Solar Probe Observations
Authors: Gabor Toth, Marco Velli, Bart van der Holst
Figure caption: Formation and propagation of spherically polarized Alfvén waves in the spherically expanding solar wind. The top panels show the three components of the magnetic field and its magnitude in part of the 2D computational domain. The circularly polarized Alfvén waves enter through the left boundary at R = 25 R  s . The incoming radial field is perturbed along the Y-direction, which causes a shear in the Alfvén wave speed and the development of spherical polarization. Switchbacks with B  r  > 0 form at r > 27.5 R  s . The total magnetic field (top right) is relatively smooth. The black curve indicates a possible PSP trajectory at r = 31.4 R  s . The satellite symbol in the top left panel indicates a spot along the trajectory where switchbacks occur. The bottom left panels show the magnetic field and velocity components, as well as the total pressure p + p  B , magnetic pressure p  B , density n, and correlation coefficient r(B, n) between B and n over a sliding window of 0.3 R  s  along the trajectory. The virtual satellite is moving +5° longitude per day, similar to PSP near the perihelion of encounter 1. All quantities are comparable to PSP observations during the first encounter. The gradients of the total pressure are small but not zero. Density variations are also substantial and show a strong anticorrelation with the magnetic field magnitude near the switchbacks. The bottom right panels compare the magnetic (black solid lines) and velocity (red dotted lines) perturbations around a switchback. The magnetic field components are converted to Alfvén velocity components: ﹩{{\boldsymbol{V}}}_{{\rm{A}}}={\boldsymbol{B}}/\sqrt{\rho {\mu }_{0}}﹩. For the radial components, the background variation is removed with a smoothing over 100 grid cells (0.34 R  s ). All components satisfy the Alfvénic relationship to a high accuracy similar to PSP observations (Kasper et al. 2019).
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Relation among the three components of magnetic field. The top left triangle illustrates the physical quantities describing each arrow. The top right, bottom left, and bottom right triangles show the results of the cylindrical cases with H 0/R 0 = 0.1 and 0.01 and the Cartesian case, respectively. The numerical values indicate the rate of the change of magnetic energy, ﹩\tfrac{\partial \mathrm{ln}\overline{[{B}_{i}^{2}]}}{\partial t}﹩, per rotation time averaged over 25–300 rotations (See Table 2). The positive (negative) rates with ≥1 (≤ − 1) are shown by red solid (blue dashed) arrows. We note that the sum of the values on the arrows entering each B  i  is =0 when the time-steady condition is achieved.
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Comparison of the time evolutions of [α M] averaged over the simulation box for the cylindrical cases with H 0/R 0 = 0.1 (red solid) and 0.01 (blue dotted) and the Cartesian case (black dashed).
Paper: Theory of Magnetic Switchbacks Fully Supported by Parker Solar Probe Observations
Authors: Gabor Toth, Marco Velli, Bart van der Holst
Figure caption: Analysis of PSP observations to check the satisfaction of Equation (1). The magnitude of dB  R /B ⊥ (black line) is compared with the transverse gradient of the wave speed dv/(rd α) multiplied by the time t = D/v it takes to reach PSP (red line), where D is set to match the averages of the two curves. The left column shows the results when the full time period is used. The right column shows only the bins where the magnitude of the correlation coefficient between dB  R  and B  y  is ∣r(dB  R , B  y )∣ > 0.5. The top and bottom rows are for encounters 1 and 12, respectively. The number of bins N, Pearson’s correlation r, Spearman’s rank correlation r  s , and statistical significance (p-value) p are shown in the top left corner of each plot.
Paper: Theory of Magnetic Switchbacks Fully Supported by Parker Solar Probe Observations
Authors: Gabor Toth, Marco Velli, Bart van der Holst
Figure caption: Formation of switchbacks due to different causes of the wave velocity shear. The top panels show the variation of the radial velocity u  r , radial field B  r , and density n and the resulting variation in the wave velocity v = u  r  + V A along y at t = 0. The first three columns have perturbations of the wave velocity due to perturbations in u  r , B  r , and n, respectively. The fourth column has perturbations in both u  r  and B  r  that cancel each other out, so v is constant. The bottom panels show B  r  (colors) with white field lines in the region with maximum shear at various times. The simulations in the first three panels produce switchbacks, B  r  < 0 (red stripes), but the fourth does not because there is no shear in v.
Paper: MHD in a Cylindrical Shearing Box. II. Intermittent Bursts and Substructures in MRI Turbulence
Authors: Takeru K. Suzuki
Figure caption: Comparison of the volume-integrated averages of the variation rates in magnetic energy (Equations (21)–(23) and Table 2) of the cylindrical case with H 0/R 0 = 0.1 (left) and the Cartesian case (right). What are shown from top to bottom are ﹩\tfrac{\partial \mathrm{ln}{[{B}_{R}]}^{2}}{\partial t}﹩ (or ﹩\tfrac{\partial \mathrm{ln}{[{B}_{x}]}^{2}}{\partial t}﹩), ﹩\tfrac{\partial \mathrm{ln}{[{B}_{\phi }]}^{2}}{\partial t}﹩ (or ﹩\tfrac{\partial \mathrm{ln}{[{B}_{y}]}^{2}}{\partial t}﹩), and ﹩\tfrac{\partial \mathrm{ln}{[{B}_{z}]}^{2}}{\partial t}﹩ in units of (rotation time)−1. Smoothing with spline interpolation is applied to the plotted lines to display the long-time evolution. By this treatment, the original numerical data are averaged over ≈3 rotation times.