adsabs/AstroCLIMB huggingface dataset:
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: (a) Distribution of dust grain distances from the planet over time for an impulsive dust ejection event. The colored curves represent different numbers of elapsed orbits since the release. Values of β are drawn from a uniform distribution ﹩{ \mathcal U }﹩, while H denotes the Heaviside function. (b) A steady-state dust tail profile, shown as the integral of the dust distribution over time weighted by a decay function G(N), characterized by a scale number N0. The decaying profiles both use N0 = 2, specifically chosen such that the resulting decay of the dust density visually resembles plausible transit profiles of BD+05 4868 A in Figure 8.
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: Properties of the single transit observed with LCOGT multiwavelength photometry. The points are plotted at approximately the central wavelength of the four MuSCAT3 bandpasses. (a) A comparison of measured transit depths across the four LCO bandpasses. (b) Integrated area beneath each LCOGT light curve (Atot,LCO) relative to that measured from TESS (Atot,TESS). The total absorption is the integrated area beneath the model transit profile ﹩{ \mathcal T }(\phi )﹩ that is fit to the observed data.
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: (a)–(b) Light curves of BD+05 4868 A from the All-Sky Automated Survey for Supernovae (ASAS-SN) folded at a period of 1.271869 days at the ephemerides determined from TESS data. The ASAS-SN light curves are binned over 75 minute intervals. The shaded bands indicate the formal and binned flux uncertainties added in quadrature. (c) A comparison between the TESS and ASAS-SN phase-folded light curves.
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: Trajectories of simulated dust grains as viewed in the x − y plane, with each trajectory colored by the β value of its corresponding grain. The parameters of this simulation are similar to those presented in Figure 11, except that the trajectories here are numerically integrated across only five orbits, and the grains are not allowed to decay.
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: Simulated contributions to the transit profile. The black, orange, blue, and red curves are the dust extinction profile, the absorption profile of the transit, the forward scattering peak, and the net observed transit profile. These results were computed using a representative value of r/λ = 6, and are generally insensitive to varying r/λ between 1 and 10.
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: Detection limits of the NEID radial velocity (RV) observations in Section 4.1, below which the RV data is insensitive to the presence of a companion to BD+05 4868 A. Shown are curves for three orbital inclination angles (i) of the companion. The spikes at 1 and 2 days are caused by the RV observations being taken at increments of a day.
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: Near-infrared adaptive optics imaging and corresponding sensitivity curves for BD+05 4868 A in (a) the narrowband J continuum (Jcont) and in (b) the narrowband K continuum (Kcont). The increased uncertainty at Δarcsec ∼ 3﹩\mathop{.}\limits^{\unicode{x02033}}﹩0 is caused by the presence of BD+05 4868 B.
Paper: exoALMA. II. Data Calibration and Imaging Pipeline
Authors: Ryan A. Loomis, Stefano Facchini, Myriam Benisty, Pietro Curone, John D. Ilee, Gianni Cataldi, Hsi-Wei Yen, Richard Teague, Christophe Pinte, Jane Huang, Himanshi Garg, Ryuta Orihara, Ian Czekala, Brianna Zawadzki, Sean M. Andrews, David J. Wilner, Jaehan Bae, Marcelo Barraza-Alfaro, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Example of improvement of phase coherence. Visibility amplitude ratio as a function of the deprojected baselines for PDS 66 between LB EB0 and LB EB1 (reference) at different rounds of SB+LB self-calibration after flux rescaling.
Paper: exoALMA. II. Data Calibration and Imaging Pipeline
Authors: Ryan A. Loomis, Stefano Facchini, Myriam Benisty, Pietro Curone, John D. Ilee, Gianni Cataldi, Hsi-Wei Yen, Richard Teague, Christophe Pinte, Jane Huang, Himanshi Garg, Ryuta Orihara, Ian Czekala, Brianna Zawadzki, Sean M. Andrews, David J. Wilner, Jaehan Bae, Marcelo Barraza-Alfaro, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Example of flux offset even after phase self-calibration. Visibility amplitude ratio as a function of the deprojected baseline for PDS 66 at the last round of SB+LB phase self-calibration of iteration 1 (left, without applying flux rescaling) and iteration 2 (right, after applying flux rescaling).
Paper: exoALMA. II. Data Calibration and Imaging Pipeline
Authors: Ryan A. Loomis, Stefano Facchini, Myriam Benisty, Pietro Curone, John D. Ilee, Gianni Cataldi, Hsi-Wei Yen, Richard Teague, Christophe Pinte, Jane Huang, Himanshi Garg, Ryuta Orihara, Ian Czekala, Brianna Zawadzki, Sean M. Andrews, David J. Wilner, Jaehan Bae, Marcelo Barraza-Alfaro, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Demonstration of the improvements on the imaging quality of the continuum emission of LkCa 15 after the application of self-calibration on (1) just the ACA data, (2) ACA+SB data, and (3) ACA+SB+LB data.
Paper: exoALMA. II. Data Calibration and Imaging Pipeline
Authors: Ryan A. Loomis, Stefano Facchini, Myriam Benisty, Pietro Curone, John D. Ilee, Gianni Cataldi, Hsi-Wei Yen, Richard Teague, Christophe Pinte, Jane Huang, Himanshi Garg, Ryuta Orihara, Ian Czekala, Brianna Zawadzki, Sean M. Andrews, David J. Wilner, Jaehan Bae, Marcelo Barraza-Alfaro, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Improvement of waterfalls in PDS 66 after flux rescaling (correlation XX, uv-range: 125–150 m).
Paper: exoALMA. II. Data Calibration and Imaging Pipeline
Authors: Ryan A. Loomis, Stefano Facchini, Myriam Benisty, Pietro Curone, John D. Ilee, Gianni Cataldi, Hsi-Wei Yen, Richard Teague, Christophe Pinte, Jane Huang, Himanshi Garg, Ryuta Orihara, Ian Czekala, Brianna Zawadzki, Sean M. Andrews, David J. Wilner, Jaehan Bae, Marcelo Barraza-Alfaro, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Representative exoALMA imaging workflow shown for a single channel of the 12CO 3–2 cube for MWC 758.
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: 3D simulation of 50,000 dust grains in the corotating frame of the orbiting planet, integrated for up to 30 planetary orbits. The host star is shown to scale, while the planet’s size is inflated by a factor of 50 in panels (a) and (c) for visual clarity. (a) A view from above the planetary orbit, looking down at the x − y plane in which the planet is orbiting counterclockwise. The trails indicate the accumulated trajectories of the dust grains over time. There are two distinct trails that correspond to the leading and trailing dust tails. (b) A view of the accumulated trajectories of the dust tails in the z − ϕ plane (an “unrolled” dust tail), showing the azimuthal extent of the tails. For comparison, the subpanel beneath the color image shows the absorption profiles of the leading and trailing tails, which are based on fitting the mean transit profile ﹩{ \mathcal T }(\phi )﹩ to the TESS data in Figure 7. (c) Visualization of the simulated dust tails projected onto the z − y plane, with the host star shown in the background to demonstrate the extent of the dust tail’s height. (d) A close-in view of the dust tail in the x − y plane. Tracks correspond to trajectories of individual grains as they are launched from the boundary of the Hill “sphere” of the planet. The region in cyan represents the outflowing Parker wind. Each grain is assigned a β value, which influences its trajectory and whether it ends up in the leading or the trailing tail.
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: Measured properties from the fitting of individual transits from the TESS light curves in Figure 8, with a similar labeling scheme for the transit number. The vertical lines indicate gaps within the light curve; double lines indicate the gap between Sectors 55 and 82. The errors are computed from the 16th and 84th percentiles of the posterior distribution from model fits of ﹩{ \mathcal Y }(d)﹩. (a) The total integrated area under the extinction profiles of each transit (Atot), normalized by the corresponding value from the mean transit profile (Atot,mean). (b) Ratio of the integrated area under the trailing tail’s extinction profile with that from the leading tail. (c) Ratio of generalized-Gaussian scale lengths between the trailing and leading tails. (d) The trailing tails’ e-folding length in units of ϕ, assuming an exponential decay. (e) Transit depth, measured as the minimum flux level in the transit profile.
Paper: exoALMA. II. Data Calibration and Imaging Pipeline
Authors: Ryan A. Loomis, Stefano Facchini, Myriam Benisty, Pietro Curone, John D. Ilee, Gianni Cataldi, Hsi-Wei Yen, Richard Teague, Christophe Pinte, Jane Huang, Himanshi Garg, Ryuta Orihara, Ian Czekala, Brianna Zawadzki, Sean M. Andrews, David J. Wilner, Jaehan Bae, Marcelo Barraza-Alfaro, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: uv-coverage of the LkCa 15 data set. The visibilities in the plot are binned in 30 s intervals. Three LB EBs were executed back-to-back, yielding optimal hour angle spanning and uv-coverage for such a low-elevation source. Note that the final combined uv-coverage results in a PSF that is non-Gaussian (see, e.g., I. Czekala et al. 2021), discussed further in 4.1.
Paper: exoALMA. II. Data Calibration and Imaging Pipeline
Authors: Ryan A. Loomis, Stefano Facchini, Myriam Benisty, Pietro Curone, John D. Ilee, Gianni Cataldi, Hsi-Wei Yen, Richard Teague, Christophe Pinte, Jane Huang, Himanshi Garg, Ryuta Orihara, Ian Czekala, Brianna Zawadzki, Sean M. Andrews, David J. Wilner, Jaehan Bae, Marcelo Barraza-Alfaro, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Example of the exoALMA spatial alignment procedure on J1604 between LB1 and LB2 (the reference EB). The panels show the dust continuum images before any self-calibration or alignment (a and b), after the individual EB self-calibration (c and d), and after the alignment (e and f, with e = c since LB2 is the reference EB and, thus, is not shifted). The contours on c, d, e, and f indicate the 5σ level in c and e. The rms values were calculated in an annulus between 3″ and 4″ centered on the disk. The rightmost column presents the image ratio of the two EBs before and after alignment (g = d/c and h = f/e) with a mask showing regions with SNR > 3 in LB2. These plots highlight the successful alignment for a target that lacks a centrally peaked emission, making it unsuitable for the classical image-plane Gaussian fitting.
Paper: exoALMA. II. Data Calibration and Imaging Pipeline
Authors: Ryan A. Loomis, Stefano Facchini, Myriam Benisty, Pietro Curone, John D. Ilee, Gianni Cataldi, Hsi-Wei Yen, Richard Teague, Christophe Pinte, Jane Huang, Himanshi Garg, Ryuta Orihara, Ian Czekala, Brianna Zawadzki, Sean M. Andrews, David J. Wilner, Jaehan Bae, Marcelo Barraza-Alfaro, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Schematic of the spatial alignment workflow of the exoALMA collaboration. The top histograms represent the distribution in uv baseline distances for each of the three configurations considered, with the longest baselines to the left. The order of operations starts in the top left and moves to the bottom right. Note that this is the inverse of our ACA-first self-calibration order of operations, with both being intentional.
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: Same as Figure 11, but using different initial launch parameters for the dust grains. In the top row, the grains are simulated to form only at a distance past the Hill sphere by setting β = 0 for half of the first orbit after release. In the bottom panel, the grains are released from the surface of a 0.02M⊕ planet with a radius of 2000 km with a velocity corresponding to the planet’s escape velocity (in isolation) of 3 km s−1.
Paper: exoALMA. II. Data Calibration and Imaging Pipeline
Authors: Ryan A. Loomis, Stefano Facchini, Myriam Benisty, Pietro Curone, John D. Ilee, Gianni Cataldi, Hsi-Wei Yen, Richard Teague, Christophe Pinte, Jane Huang, Himanshi Garg, Ryuta Orihara, Ian Czekala, Brianna Zawadzki, Sean M. Andrews, David J. Wilner, Jaehan Bae, Marcelo Barraza-Alfaro, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: exoALMA calibration workflow. Individual MOUS data sets are color coded (ACA, LB, SB) and referred to with no spacing (e.g., (ACA)SBLB) when concatenated.
Paper: exoALMA. II. Data Calibration and Imaging Pipeline
Authors: Ryan A. Loomis, Stefano Facchini, Myriam Benisty, Pietro Curone, John D. Ilee, Gianni Cataldi, Hsi-Wei Yen, Richard Teague, Christophe Pinte, Jane Huang, Himanshi Garg, Ryuta Orihara, Ian Czekala, Brianna Zawadzki, Sean M. Andrews, David J. Wilner, Jaehan Bae, Marcelo Barraza-Alfaro, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Gaylor Wafflard-Fernandez, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Visibility amplitude (left) and visibility amplitude ratio relative to LB1 (right) as a function of the deprojected baselines for PDS 66 after self-calibration of individual EBs, alignment, and flux rescaling but before group self-calibration, demonstrating misalignment between the EBs due to decorrelation from remaining phase errors.
Paper: A Disintegrating Rocky Planet with Prominent Comet-like Tails around a Bright Star
Authors: Marc Hon, Saul Rappaport, Avi Shporer, Andrew Vanderburg, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Khalid Barkaoui, Samuel W. Yee, Joshua N. Winn, Alex S. Polanski, Emily A. Gilbert, David R. Ciardi, Jeroen Audenaert, William Fong, Jack Haviland, Katharine Hesse, Daniel Muthukrishna, Glen Petitpas, Ellie Hadjiyska Schmelzer, Norio Narita, Akihiko Fukui, Sara Seager, George R. Ricker
Figure caption: Corner plot of the posterior distribution to the fit to the mean transit profile of BD+05 4868 A’s TESS light curve.
Paper: The Ubiquity of Twisted Flux Ropes in the Quiet Sun
Authors: Tahar Amari, Aurélien Canou, Marco Velli, Zoran Mikic, Frederic Alauzet, Eric Buchlin, Jean-François Luciani, Jean-Jacques Aly, Lucas A. Tarr
Figure caption: (a) Boxes enclosing TFRs used to compute some of their characteristics. Each box can contain one or a few TFRs when difficult to isolate. (b) Magnetic twist at z = 1, Mm. (c) Synthetic emissivity from the electric current density. Below panel (a) are listed values of Wtot and Wpot, the magnetic energy of the reconstructed solution and the current-free one for the entire magnetogram; W, the magnetic energy contained in each box; ΔW, the free magnetic energy (compared to the current-free field); Wsop, the semiopen field energy associated with the opening of each box; and ∣Tw∣, the magnetic twist of the TFR in each box (or the maximum when several are present). All magnetic energies are expressed in ergs.
Paper: The Ubiquity of Twisted Flux Ropes in the Quiet Sun
Authors: Tahar Amari, Aurélien Canou, Marco Velli, Zoran Mikic, Frederic Alauzet, Eric Buchlin, Jean-François Luciani, Jean-Jacques Aly, Lucas A. Tarr
Figure caption: Hinode/SOT high-resolution photospheric magnetic map used to build up adapted resolution boundary conditions. (a) The normal component Bz of the magnetic field for the full-size magnetogram (216 × 114 Mm2), from which we extract a subdomain (solid line rectangle) of 96 × 70 Mm2 corresponding to the domain above which the coronal magnetic field is reconstructed, and within which a smaller one (dashed line) corresponds to the domain of simulation (15 × 15 Mm2). (b) Zoom on the normal component Bz for the reconstruction domain. (c) Continuum image for the reconstruction domain exhibiting the granulation scale. (d) The normal component Jz of the electric current for the reconstruction domain.
Paper: The Ubiquity of Twisted Flux Ropes in the Quiet Sun
Authors: Tahar Amari, Aurélien Canou, Marco Velli, Zoran Mikic, Frederic Alauzet, Eric Buchlin, Jean-François Luciani, Jean-Jacques Aly, Lucas A. Tarr
Figure caption: Selected field lines of the magnetic environment above the photosphere during the simulation, taken at two different times and two different view angles. TFRs appear around mesospots and below and above the transition regions. The horizontal size of the domain is the same as that of the smallest rectangle drawn in green in Figure 1. Both views provide a horizontal scalar map of the vertical component of the magnetic field in the high chromosphere.
Paper: The Ubiquity of Twisted Flux Ropes in the Quiet Sun
Authors: Tahar Amari, Aurélien Canou, Marco Velli, Zoran Mikic, Frederic Alauzet, Eric Buchlin, Jean-François Luciani, Jean-Jacques Aly, Lucas A. Tarr
Figure caption: Selected field lines of the magnetic environment above the photosphere using the force-free model XTRAPOL. TFRs stand around mesospots, both below and above the transition regions. The red rectangle shown on the right features the same box size as the one of the simulation box considered in Section 3.