adsabs/AstroCLIMB huggingface dataset:
Paper: Metallicities of Classical Cepheids in the Inner Galactic Disk
Authors: Noriyuki Matsunaga, Daisuke Taniguchi, Scarlet S. Elgueta, Takuji Tsujimoto, Junichi Baba, Andrew McWilliam, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi, Haruki Katoh, Satoshi Hamano, Yuji Ikeda, Hideyo Kawakita, Charlie Hull, Rogelio Albarracín, Giuseppe Bono, Valentina D'Orazi
Figure caption: The metallicity distribution of Cepheids plotted against (a) R GC, (b) l, and (c) β. The red circles indicate our results, while the other symbols indicate the results from some relevant papers—Luck (2018) with gray circles, Kovtyukh et al. (2022) with blue crosses, Elgueta (2022) with red diamonds, and Trentin et al. (2023) with blue circles. The error bars for our measurements include the systematic errors, while those for Kovtyukh et al. (2022) and Elgueta (2022) include the standard deviation of line-by-line [Fe/H] only. The black triangles in panel (a) show the averaged metallicity of the Cepheids from Luck (2018) in bins with a width of 1 kpc at each position. The linear regression to the metallicity gradient is indicated by the red line, together with the 90% confidence interval for our Cepheids, while the black counterpart indicates the gradient obtained for the Cepheids from Luck (2018) at R GC > 6.5 kpc. In panels (b) and (c), only the objects in the inner disk (3 < R GC < 6.5 kpc) are compared.
Paper: Metallicities of Classical Cepheids in the Inner Galactic Disk
Authors: Noriyuki Matsunaga, Daisuke Taniguchi, Scarlet S. Elgueta, Takuji Tsujimoto, Junichi Baba, Andrew McWilliam, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi, Haruki Katoh, Satoshi Hamano, Yuji Ikeda, Hideyo Kawakita, Charlie Hull, Rogelio Albarracín, Giuseppe Bono, Valentina D'Orazi
Figure caption: Velocities of Cepheids plotted against the Galactic longitude.
Paper: Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429
Authors: Yusuke Aso, Woojin Kwon, Nagayoshi Ohashi, Jes K. Jørgensen, John J. Tobin, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Patrick M. Koch, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Jinshi Sai (Insa Choi), Kazuya Saigo, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams, Hsi-Wei Yen
Figure caption: Images of the 1.3 mm continuum emission produced with (a) the robust parameter of 0.0 and no taper, (b) the robust parameter of −2.0 and a 3 Mλ (∼0.″06) taper, (c) the robust parameter of 2.0 and a 1 Mλ (∼0.″18) taper. The brightness temperature T  b  is calculated from the Rayleigh–Jeans approximation. The contour levels are 3σ, 6σ, 12σ, 24σ, 48σ, 96σ, and 192σ, where 1σ is (a) 0.022, (b) 0.100, and (c) 0.023 mJy beam−1 (Table 1). The filled ellipses at the bottom-left corners denote the synthesized beams: (a) 0.″073 × 0.″048 (77°), (b) 0.″043 × 0.″034 (73°), and (c) 0.″29 × 0.″24 (86°). The diagonal lines denote the major and minor axes of the emission in the image in panel (a): P.A. = 113° and 23°. The square in panel (a) shows the plotted range of panel (b).
Paper: Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429
Authors: Yusuke Aso, Woojin Kwon, Nagayoshi Ohashi, Jes K. Jørgensen, John J. Tobin, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Patrick M. Koch, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Jinshi Sai (Insa Choi), Kazuya Saigo, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams, Hsi-Wei Yen
Figure caption: Moment 0 and 1 maps in the SO J  N  = 65−54 line emission. The contour maps show the moment 0 map, while the color images show the moment 1 map. (a) The robust parameter is 0.5. The emission is integrated from 1.7 to 6.3 km s−1. The contour levels are in 3σ steps from 3σ with 1σ = 2.3 mJy beam−1 km s−1. The beam size is 0.″18 × 0.″14 (87°). (b) The robust parameter is 2. The emission is integrated from 1.7 to 6.3 km s−1. The contour levels are in 3σ steps from 3σ until 15σ and then in 10σ steps with 1σ = 2.1 mJy beam−1 km s−1. The beam size is 0.″37 × 0.″26 (78°). The diagonal lines are the major and minor axes of the continuum emission, P.A. = 113° and 23°.
Paper: Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429
Authors: Yusuke Aso, Woojin Kwon, Nagayoshi Ohashi, Jes K. Jørgensen, John J. Tobin, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Patrick M. Koch, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Jinshi Sai (Insa Choi), Kazuya Saigo, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams, Hsi-Wei Yen
Figure caption: Moment 0 (integrated intensity) and 1 (mean velocity) maps in the 12CO J = 2–1 line. The contour maps show the moment 0 map, while the color images show the moment 1 map. (a) Moment maps with the robust parameter of 2.0, integrated from V LSR = −6.0 to 14.0 km s−1. (b) Zoom-in view of the moment maps with the robust parameter of 0.5, integrated from V LSR = −6.0 to 14.0 km s−1. The contour levels are in (a) 12σ steps from 12σ with 1σ = 3.2 mJy beam−1 km s−1 and (b) 6σ steps from 6σ with 1σ = 3.5 mJy beam−1 km s−1. The filled ellipse at the bottom-left corner shows the synthesized beam: (a) 0.″35 × 0.″25 (76°) and (b) 0.″17 × 0.″13 (88°). The diagonal lines are the major and minor axes of the continuum emission, P.A. = 113° and 23°. The green contour in panel (b) shows the 5σ level of the continuum emission (Figure 1(a)).
Paper: Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429
Authors: Yusuke Aso, Woojin Kwon, Nagayoshi Ohashi, Jes K. Jørgensen, John J. Tobin, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Patrick M. Koch, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Jinshi Sai (Insa Choi), Kazuya Saigo, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams, Hsi-Wei Yen
Figure caption: Moment 0 and 1 maps in the C18O J = 2–1 line emission and the 13CO J = 2–1 line emission. The contour maps show the moment 0 map, while the color images show the moment 1 map. The contour levels are in 3σ steps in the robust = 0.5 images and 6σ steps in the robust = 2 images starting from 3σ. The C18O emission is integrated from 0.8 to 7.1 km s−1. These moment 0 maps have 1σ of 2.2 (robust = 0.5) and 2.0 mJy beam−1 km s−1 (robust = 2). The 13CO emission is integrated from 0.7 to 7.3 km s−1. These moment 0 maps have 1σ of 2.8 (robust = 0.5) and 2.7 mJy beam−1 km s−1 (robust = 2). The beam sizes are (a) 0.″18 × 0.″14 (87°), (b) 0.″38 × 0.″27 (78°) (c) 0.″17 × 0.″13 (87°), and (d) 0.″37 × 0.″26 (77°). The diagonal lines are the major and minor axes of the continuum emission, P.A. = 113° and 23°.
Paper: Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429
Authors: Yusuke Aso, Woojin Kwon, Nagayoshi Ohashi, Jes K. Jørgensen, John J. Tobin, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Patrick M. Koch, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Jinshi Sai (Insa Choi), Kazuya Saigo, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams, Hsi-Wei Yen
Figure caption: PV diagram in the 12CO J = 2–1 line along the outflow axis (P.A. = 23°) with a width of 0.″6. The positive offset corresponds to the northern side. The contour levels are in 6σ steps from 6σ, where 1σ is 0.85 mJy beam−1. The dashed lines denote the systemic velocity (V LSR = 4 km s−1) and the protostellar position. The orange short lines denote the position of local peaks or extensions visually identified.
Paper: Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429
Authors: Yusuke Aso, Woojin Kwon, Nagayoshi Ohashi, Jes K. Jørgensen, John J. Tobin, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Patrick M. Koch, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Jinshi Sai (Insa Choi), Kazuya Saigo, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams, Hsi-Wei Yen
Figure caption: Comparison between the predicted maximum line-of-sight velocities (white dashed and dotted curves) and the observed PV diagrams (C18O in red, SO in green, and 12CO in blue). (a) PV diagram along the major axis. The dashed curves represent the UCM envelope model with a central stellar mass of M * = 0.14 M ☉ (Section 4.2) and the specific angular momentum j = 45 km s−1 au (Hsieh et al. 2019a). The envelope maximum velocity is calculated only up to ∣V−V sys∣ = 2 km s−1. The dotted curves show the maximum line-of-sight velocities of the Keplerian disk with a disk radius of 16 au. (b) PV diagram along the minor axis. The dashed curves represent the same UCM envelope as that of the major axis.
Paper: Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429
Authors: Yusuke Aso, Woojin Kwon, Nagayoshi Ohashi, Jes K. Jørgensen, John J. Tobin, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Patrick M. Koch, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Jinshi Sai (Insa Choi), Kazuya Saigo, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams, Hsi-Wei Yen
Figure caption: Edge and ridge points, estimated for each velocity channel, overlaid on the 12CO major-axis PV diagram (robust = 0.5) in the (a) linear and (b) logarithmic scales. The positive radius corresponds to the western side. The velocity is the relative velocity to the systemic velocity of V LSR = 4 km s−1. The white curves/lines are the best-fit power-law functions (Section 4.2). The contour levels are in the 3σ steps from 3σ, where 1σ is 1.4 mJy beam−1.
Paper: Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429
Authors: Yusuke Aso, Woojin Kwon, Nagayoshi Ohashi, Jes K. Jørgensen, John J. Tobin, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Patrick M. Koch, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Jinshi Sai (Insa Choi), Kazuya Saigo, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams, Hsi-Wei Yen
Figure caption: Schematic picture of the Keplerian disk, ring, envelope, streamer, outflow identified in the CO isotopologue and SO lines, and the eastern excess in the 1.3 mm continuum emission in the Class 0 protostar IRAS 16253-2429. The gray background represents the large-scale envelope identified in 8 μm extinction (Tobin et al. 2010). The radii or lengths for each of the structures are indicated as well in units of astronomical units.
Paper: Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429
Authors: Yusuke Aso, Woojin Kwon, Nagayoshi Ohashi, Jes K. Jørgensen, John J. Tobin, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Patrick M. Koch, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Jinshi Sai (Insa Choi), Kazuya Saigo, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams, Hsi-Wei Yen
Figure caption: (a) Axisymmetric model (red) fitted to the observed 1.3 mm continuum emission (black) with the robust parameter of 0.0. The contour levels are the same as Figure 1(b): 3σ, 6σ, 12σ, 24σ, 48σ, 96σ, and 192σ. (b) Residual (contour map) between the model and observation in panel (a), overlaid on the robust = −2 continuum image (color map; Figure 1(c)). The contour levels are the same: 3σ, 6σ, 12σ, and 24σ.
Paper: Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429
Authors: Yusuke Aso, Woojin Kwon, Nagayoshi Ohashi, Jes K. Jørgensen, John J. Tobin, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Patrick M. Koch, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Jinshi Sai (Insa Choi), Kazuya Saigo, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams, Hsi-Wei Yen
Figure caption: Ridge points, found for each velocity, overlaid on the SO PV diagram (robust = 2) along the major axis in the linear scale. The positive radius corresponds to the western side. The velocity is relative to the systemic velocity of V LSR = 4 km s−1. The white line is the best linear function (Section 4.3). The contour levels are in the 3σ steps from 3σ, where 1σ is 2.3 mJy beam−1.
Paper: Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429
Authors: Yusuke Aso, Woojin Kwon, Nagayoshi Ohashi, Jes K. Jørgensen, John J. Tobin, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Patrick M. Koch, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Jinshi Sai (Insa Choi), Kazuya Saigo, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams, Hsi-Wei Yen
Figure caption: PV diagrams in the 12CO (blue; robust = 0.5), C18O (red; robust = 2.0), and 13CO (color; robust = 2.0) J = 2–1 lines along the (a) major and (b) minor axes. The positive offset corresponds to the western and northern sides in panels (a) and (b), respectively. The contour levels are in 6σ steps from 6σ, where 1σ is 1.4 mJy beam−1 for 12CO, 2.1 mJy beam−1 for C18O, and 3.0 mJy beam−1 for 13CO. The beam sizes in these diagrams are ∼0.″15 for 12CO, ∼0.″33 for C18O, and ∼0.″32 for 13CO (Table 1).
Paper: Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429
Authors: Yusuke Aso, Woojin Kwon, Nagayoshi Ohashi, Jes K. Jørgensen, John J. Tobin, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Patrick M. Koch, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Jinshi Sai (Insa Choi), Kazuya Saigo, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams, Hsi-Wei Yen
Figure caption: Model map of the line-of-sight velocity of a streamer in the UCM envelope (M * = 0.14 M ☉ and j = 45 km s−1 au are the same as for Figure 11) and a Keplerian ring at 28 au. The streamer comes from 30° above the midplane (i.e., θ 0 = 60°) and 0°–20° away from the left to the front seen by the observer around the rotational axis (i.e., ϕ 0 = 240°–270°).
Paper: Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429
Authors: Yusuke Aso, Woojin Kwon, Nagayoshi Ohashi, Jes K. Jørgensen, John J. Tobin, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Patrick M. Koch, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Jinshi Sai (Insa Choi), Kazuya Saigo, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams, Hsi-Wei Yen
Figure caption: Moment 0 and 1 maps in five other molecular lines (nine transitions) observed in the ALMA observations of the eDisk project. These images are made with the robust parameter of 2. The emission is integrated from 2.66 to 5.34 km s−1 (three channels) for all lines. The contour levels are in 3σ steps from 3σ, where 1σ is 1.5 mJy beam−1 km s−1. The ellipse in the lower left corner of each panel denotes the synthesized beam, ∼0.″38 × 0.″27 (78°). The diagonal lines are the major and minor axes of the continuum emission, P.A. = 113° and 23°.
Paper: Early Planet Formation in Embedded Disks (eDisk). VI. Kinematic Structures around the Very-low-mass Protostar IRAS 16253-2429
Authors: Yusuke Aso, Woojin Kwon, Nagayoshi Ohashi, Jes K. Jørgensen, John J. Tobin, Yuri Aikawa, Itziar de Gregorio-Monsalvo, Ilseung Han, Miyu Kido, Patrick M. Koch, Shih-Ping Lai, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Leslie W. Looney, Suchitra Narayanan, Nguyen Thi Phuong, Jinshi Sai (Insa Choi), Kazuya Saigo, Alejandro Santamaría-Miranda, Rajeeb Sharma, Shigehisa Takakuwa, Travis J. Thieme, Kengo Tomida, Jonathan P. Williams, Hsi-Wei Yen
Figure caption: Corner plot of the MCMC fitting to the continuum image. Two angles, i and P.A., are plotted among the 14 free parameters. The dashed lines show the 16th, 50th, and 84th percentiles.
Paper: Electron Acceleration and Heating during Magnetic Reconnection in the Earth's Quasi-parallel Bow Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: (a)–(c) Time evolution of current density J  z . Black curves are magnetic field lines. The white vertical line in each plot shows the position of the maximum 〈B  y 〉 (the y average of B  y ), which roughly indicates the position of the shock plane. Three ion-scale magnetic islands are denoted by numbers 1–3. (d) Profiles of 〈B  y 〉, which is B  y  averaged over y. The arrows show the same positions of the white line in each of panels (a)–(c). (e) 2D field lines at Ω i  t = 20.31, and two lines, y = 20d  i  and y = 18d  i , along which 1D cuts of B  y  are shown in panel (f). The position of an X line is denoted by X. (f) 1D cuts of B  y  along y = 20d  i  (thick blue) and y = 18d  i  (black). The thin blue curve shows 〈B  y 〉.
Paper: Electron Acceleration and Heating during Magnetic Reconnection in the Earth's Quasi-parallel Bow Shock
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz
Figure caption: Contours of the y-component of the ion fluid velocity V  iy  and the electron fluid velocity V  ey . Magenta lines are magnetic field lines. Island 2 is the same ion-scale island as in Figure 1. The blue X mark and the red X mark show the positions of reconnection X lines associated with ion-coupled reconnection and electron-only reconnection, respectively. In panels (a) and (b), the regions with black ovals are where jets are generated. White arrows show the velocity vectors. (c) In grayscale, the in-plane speed of ion fluid, ﹩{({V}_{{ix}}^{2}+{V}_{{iy}}^{2})}^{1/2}﹩ is shown. (d) In grayscale, the in-plane speed of electron fluid, ﹩{({V}_{{ex}}^{2}+{V}_{{ey}}^{2})}^{1/2}﹩, multiplied by the sign of V  ey  is shown. Only the regions with positive V  ey  are shown in grayscale, and the regions with negative V  ey  are in white. In both panels (c) and (d), magenta arrows represent the fluid velocity vectors, and the blue and red oval regions are around the blue X line and the red X line, respectively.
Paper: Avalanches and the Distribution of Reconnection Events in Magnetized Circumstellar Disks
Authors: Marco Fatuzzo, Fred C. Adams, Adina D. Feinstein, Darryl Z. Seligman
Figure caption: Frequency distributions of the avalanche total energy N  E  for the fast reconnection model (red curve), slow reconnection model with uniform perturbation structure (maroon curve), and slow reconnection model with sheared perturbation structure (pink curve). We show the corresponding distributions for duration N  t  and power N  P  in green (middle) and purple (bottom), respectively, as well. In each panel, the dashed black line represents the corresponding power-law fit from Lu et al. (1993).
Paper: Avalanches and the Distribution of Reconnection Events in Magnetized Circumstellar Disks
Authors: Marco Fatuzzo, Fred C. Adams, Adina D. Feinstein, Darryl Z. Seligman
Figure caption: Smooth component of the critical magnetic field B  y  for our baseline model. The left panel shows a cut along the x–z plane, and the right panel shows a cut along the y–z plane.
Paper: Avalanches and the Distribution of Reconnection Events in Magnetized Circumstellar Disks
Authors: Marco Fatuzzo, Fred C. Adams, Adina D. Feinstein, Darryl Z. Seligman
Figure caption: Number of trigger events for cells along an x–y plane slice for which n  z  = 25. (a) Fast reconnection model without the sheared perturbation structure. (b) Fast reconnection model with the sheared perturbation structure. The color corresponds to number of events.
Paper: Avalanches and the Distribution of Reconnection Events in Magnetized Circumstellar Disks
Authors: Marco Fatuzzo, Fred C. Adams, Adina D. Feinstein, Darryl Z. Seligman
Figure caption: A schematic diagram of the physical situation investigated in this paper.
Paper: An Unsupervised Machine Learning-based Algorithm for Detecting Weak Impulsive Narrowband Quiet Sun Emissions and Characterizing Their Morphology
Authors: Shabbir Bawaji, Ujjaini Alam, Surajit Mondal, Divya Oberoi, Ayan Biswas
Figure caption: Unsupervised clustering of the identified features using t-SNE+DBSCAN for the 120.52 MHz quiet Sun data set, represented in the t-SNE variables V 1, V 2. Each color represents a group of features that have been found to have similar properties by the algorithm. We chose three of these groups, Group 1 (blue), Group 2 (orange), Group 3 (gray), for further study.
Paper: An Unsupervised Machine Learning-based Algorithm for Detecting Weak Impulsive Narrowband Quiet Sun Emissions and Characterizing Their Morphology
Authors: Shabbir Bawaji, Ujjaini Alam, Surajit Mondal, Divya Oberoi, Ayan Biswas
Figure caption: Distribution of various attributes for three chosen groups from Figure 9. The left-hand panel shows the histograms for the maximum distance between the feature peak in a given cluster to the largest closed contour around it. The middle panel shows the histograms for the angle of orientation of the largest closed contour around the feature. The right-hand panel shows the distributions in the eccentricity of the largest closed contours against the drop in intensity from the feature to the farthest edge of the contour around it.
Paper: An Unsupervised Machine Learning-based Algorithm for Detecting Weak Impulsive Narrowband Quiet Sun Emissions and Characterizing Their Morphology
Authors: Shabbir Bawaji, Ujjaini Alam, Surajit Mondal, Divya Oberoi, Ayan Biswas
Figure caption: The left-hand panel shows the raw solar image with background noise, also referred to as the elevation map. The middle panel shows the Sobel gradient map for the same image. The boundary of the radio Sun (yellow line) is created from this map using Watershed transform to fill the areas of consistently high gradient. The right-hand panel displays the map of the Sun within the boundary defined by Sobel and Watershed methods. This boundary extends well beyond the optical disk of the Sun (white circle). This image has also been spatially aligned with other images using the moment of mass method (Section 3.2)