adsabs/AstroCLIMB huggingface dataset:
Paper: The Aligned Orbit of WASP-148b, the Only Known Hot Jupiter with a nearby Warm Jupiter Companion, from NEID and HIRES
Authors: Xian-Yu Wang, Malena Rice, Songhu Wang, Bonan Pu, Gudmundur Stefánsson, Suvrath Mahadevan, Brandon Radzom, Steven Giacalone, Zhen-Yu Wu, Thomas M. Esposito, Paul A. Dalba, Arin Avsar, Bradford Holden, Brian Skiff, Tom Polakis, Kevin Voeller, Sarah E. Logsdon, Jessica Klusmeyer, Heidi Schweiker, Dong-Hong Wu, Corey Beard, Fei Dai, Jack Lubin, Lauren M. Weiss, Chad F. Bender, Cullen H. Blake, Courtney D. Dressing, Samuel Halverson, Fred Hearty, Andrew W. Howard, Daniel Huber, Howard Isaacson, James A. G. Jackman, Joe Llama, Michael W. McElwain, Jayadev Rajagopal, Arpita Roy, Paul Robertson, Christian Schwab, Evgenya L. Shkolnik, Jason T. Wright, Gregory Laughlin
Figure caption: Spectroscopic radial velocities of WASP-148 measured with NEID (left), HIRES (center), and both together (right), as a function of orbital phase (minutes from mid-transit) along with the best-fitting R-M models shown as red dashed lines. We find a low obliquity for WASP-148b in each of the three fits. Allesfitter simultaneously fits the error scaling and each data set to weight each data set based on its likelihood. The errors of the plotted RVs are unscaled and are drawn directly from our RV pipeline. (The data used to create this figure are available.)
Paper: The Aligned Orbit of WASP-148b, the Only Known Hot Jupiter with a nearby Warm Jupiter Companion, from NEID and HIRES
Authors: Xian-Yu Wang, Malena Rice, Songhu Wang, Bonan Pu, Gudmundur Stefánsson, Suvrath Mahadevan, Brandon Radzom, Steven Giacalone, Zhen-Yu Wu, Thomas M. Esposito, Paul A. Dalba, Arin Avsar, Bradford Holden, Brian Skiff, Tom Polakis, Kevin Voeller, Sarah E. Logsdon, Jessica Klusmeyer, Heidi Schweiker, Dong-Hong Wu, Corey Beard, Fei Dai, Jack Lubin, Lauren M. Weiss, Chad F. Bender, Cullen H. Blake, Courtney D. Dressing, Samuel Halverson, Fred Hearty, Andrew W. Howard, Daniel Huber, Howard Isaacson, James A. G. Jackman, Joe Llama, Michael W. McElwain, Jayadev Rajagopal, Arpita Roy, Paul Robertson, Christian Schwab, Evgenya L. Shkolnik, Jason T. Wright, Gregory Laughlin
Figure caption: Photometric transit observations of WASP-148, obtained while simultaneously measuring the R-M effect using Keck/HIRES. In the upper panels, the model is plotted in red, while data is shown as gray dots. The residuals are provided in the lower panels. We find no significant spot-crossing signal, which would be indicative of high surface activity, during the transit. (The data used to create this figure are available.)
Paper: Multiband Electrostatic Waves below and above the Electron Cyclotron Frequency in the Near-Sun Solar Wind
Authors: Chen Shi, Jinsong Zhao, David M. Malaspina, Stuart D. Bale, Xiangcheng Dong, Tieyan Wang, Dejin Wu
Figure caption: Event overview. (a) Spectrogram of the AC-coupled differential voltage signals of V 12. (b) Spectrogram of the DC-coupled differential voltage signals of V 12. (c) The magnetic field strength ∣B∣ and magnetic field components in RTN coordinates. (d) The solar wind speed in RTN coordinates. (e) The proton number density n  p  from SPC and the electron number density estimated by using the QTN method. (f) The proton thermal temperature. (g) The electron pitch angle distribution of electrons with energy E  e  = 315 eV. The solid white curves in panels (a) and (b) denote the electron cyclotron frequency f ce. The regime permeating multiband electrostatic waves near f ce is labeled Regime I, where the time interval is from 20:00:00 UT on 2020 September 24 to 05:30:00 UT on 2020 September 25. The regime containing the two new types of electrostatic waves is labeled Regime II, where the time interval is from 08:30:00 UT to 19:30:00 UT on 2020 September 25. The times of the four typical events #1−#4 analyzed in later figures are labeled by the red dashed lines. The arrows in panel (c) indicate the position of the heliospheric current sheet (HCS).
Paper: Multiband Electrostatic Waves below and above the Electron Cyclotron Frequency in the Near-Sun Solar Wind
Authors: Chen Shi, Jinsong Zhao, David M. Malaspina, Stuart D. Bale, Xiangcheng Dong, Tieyan Wang, Dejin Wu
Figure caption: The δ E  x  and δ E  y  values of the three typical waves: (a) the first band wave in Event #1, (b) the first band wave in Event #2, and (c) the second band wave in Event #2. From top to bottom, the magnetic field components in spacecraft coordinates, the filtered δ E  x  and δ E  y  in spacecraft coordinates, the correlation coefficient ﹩{\mathrm{CC}}_{\delta {E}_{x}-\delta {E}_{y}}﹩ between δ E  x  and δ E  y , the phase difference ﹩{{\rm{\Psi }}}_{\delta {E}_{x}-\delta {E}_{y}}﹩ between δ E  x  and δ E  y , ﹩\delta {E}_{x}^{{\prime} }﹩ and ﹩\delta {E}_{y}^{{\prime} }﹩ in a frame in which ﹩{B}_{y}^{{\prime} }=0﹩ (panel (a)) and in a frame in which ﹩{B}_{x}^{{\prime} }=0﹩ (panels (b) and (c)), and hodograms for two electric field components during the time interval between two dotted lines. ﹩{\mathrm{CC}}_{\delta {E}_{x}-\delta {E}_{y}}﹩ and ﹩{{\rm{\Psi }}}_{\delta {E}_{x}-\delta {E}_{y}}﹩ are averaged over the time interval of 10/f peak, where f peak corresponds to the frequency of the power peak in each frequency band.
Paper: Multiband Electrostatic Waves below and above the Electron Cyclotron Frequency in the Near-Sun Solar Wind
Authors: Chen Shi, Jinsong Zhao, David M. Malaspina, Stuart D. Bale, Xiangcheng Dong, Tieyan Wang, Dejin Wu
Figure caption: The PSDs of the electric field components E  x  and E  y  and the wave parameters in Events #1 and #2. Panels (a1)−(c1): spectrogram of the E  x  PSD, the averaged E  x  PSD, and wave parameters including the peak, bandwidth, and amplitude in each E  x  frequency band in Event #1. Panels (d1)−(g1): spectrogram of the E  y  PSD, the averaged E  y  PSD, and wave parameters including the peak, bandwidth, and amplitude in each E  y  frequency band in Event #1. Panels (a2)−(g2) for Event #2: the description is the same as for panels (a1)−(g1). The solid and dotted white lines denote the electron cyclotron frequency f ce and the lower-hybrid frequency f LH, respectively.
Paper: Multiband Electrostatic Waves below and above the Electron Cyclotron Frequency in the Near-Sun Solar Wind
Authors: Chen Shi, Jinsong Zhao, David M. Malaspina, Stuart D. Bale, Xiangcheng Dong, Tieyan Wang, Dejin Wu
Figure caption: The PSDs of the electric field components E  x  and E  y  and the wave parameters in Event #4. Panels (a)−(g): the description is the same as those in Figure 2. The solid and dashed white curves represent the electron cyclotron frequency f ce and the ion plasma frequency f pi, respectively. Panels (h)−(k): the correlation analysis between the electric field strength ∣δ E  x,y ∣ of the f > f ce multiband electrostatic waves and the magnetic field perturbation δ B  x,y  of oblique ion-scale waves; from top to bottom panels, the waveform of ±∣δ E  x,y ∣ and δ B  x,y , the correlation coefficients ﹩{\mathrm{CC}}_{| \delta {E}_{x,y}| -\delta {B}_{x,y}}﹩, and the correlation phase differences ﹩{{\rm{\Psi }}}_{| \delta {E}_{x,y}| -\delta {B}_{x,y}}﹩.
Paper: Multiband Electrostatic Waves below and above the Electron Cyclotron Frequency in the Near-Sun Solar Wind
Authors: Chen Shi, Jinsong Zhao, David M. Malaspina, Stuart D. Bale, Xiangcheng Dong, Tieyan Wang, Dejin Wu
Figure caption: The PSDs of the electric field components E  x  and E  y  and the wave parameters in Event #3. The description of panels (a)−(g) is the same as that in Figure 2. The solid and dashed white curves represent the electron cyclotron frequency f ce and the ion plasma frequency f pi, respectively.
Paper: The Magnetic Field in the Milky Way Filamentary Bone G47
Authors: Ian W. Stephens, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Cara Battersby, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara G.S. Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Simon Coudé, Andrés Guzmán, Alyssa Goodman, Takayoshi Kusune, Fábio P. Santos, Leah Zuckerman, Frankie Encalada
Figure caption: Application of the spheroidal flux-freezing (SFF) technique (Myers et al. 2018, 2020) to the brightest cores of G47. Top left panel: contours of number density n and magnetic field direction in the midplane of the two modeled p = 2 Plummer spheroids model which have their scale length and aspect ratio fit to the column density map. The contours are n/n 0 = 0.08, 0.10, 0.15, 0.25, 0.40, 0.60, 0.90, assuming negligible background density and peak density n 0 = 7920 cm−3. The mostly horizontal magnetic field lines have spacing proportional to B −1/2. Top right panel: southwest cores of G47, rotated to be in the coordinate system of the model. Vectors are oversampled and shown for each 3.″7 pixel. The fit of the top left panel is overlaid on the image. Bottom left panel: distribution of difference in angles between observed and modeled magnetic field direction; the standard deviation is δ θ = 11°. Bottom right panel: magnetic field strengths at the same number density contours as the top left panel.
Paper: The Magnetic Field in the Milky Way Filamentary Bone G47
Authors: Ian W. Stephens, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Cara Battersby, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara G.S. Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Simon Coudé, Andrés Guzmán, Alyssa Goodman, Takayoshi Kusune, Fábio P. Santos, Leah Zuckerman, Frankie Encalada
Figure caption: Grayscale Herschel 250 μm map of G47 overlaid with inferred B-field vectors from SOFIA HAWC+ Band E (214 μm). Vectors are shown for every two pixels, oversampling the ∼5 pixels per beam. Contours show the gas column density (N gas), with levels of [0.8, 0.9, 1, 1.2, 1.5, 2, 2.5, 3, 3.5, 4] × 1022 cm−2. Red vectors are for polarization fractions (P frac) less than 0.15 while yellow vectors are for vectors with P frac between 0.15 and 1. Light red and yellow vectors indicate P frac that have signal-to-noise ratios (SNRs) between 2 and 3, while the rest of the vectors have SNRs greater than 3. Blue and green circles indicate locations of Class I and II YSOs identified by Zhang et al. (2019). The white, orange, and blue beams (bottom left, bottom right, and top right) show the FWHM resolution for the Herschel 250 μm, SOFIA, and N gas maps respectively.
Paper: The Magnetic Field in the Milky Way Filamentary Bone G47
Authors: Ian W. Stephens, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Cara Battersby, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara G.S. Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Simon Coudé, Andrés Guzmán, Alyssa Goodman, Takayoshi Kusune, Fábio P. Santos, Leah Zuckerman, Frankie Encalada
Figure caption: Coordinate system used to determine whether pixel x  c , z  c  is within a rectangle with a PA of θ, a height h, and a width w centered at x  c0, z  c0. Axes x and y are along the width and height, respectively, while x  c  − x  c0 and z  c  − z  c0 axes are along the left–right and up–down directions, respectively. Diagram is shown for x  c  = x  c0 and z  c  = z  c0.
Paper: The Magnetic Field in the Milky Way Filamentary Bone G47
Authors: Ian W. Stephens, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Cara Battersby, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara G.S. Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Simon Coudé, Andrés Guzmán, Alyssa Goodman, Takayoshi Kusune, Fábio P. Santos, Leah Zuckerman, Frankie Encalada
Figure caption: Top panel: Magnitude of the difference in angles between the bone direction and B-field direction. White empty squares show the column density spine from Zucker et al. (2018), while the black line shows the fitted polynomial to this spine. Red and black vectors are the same as Figure 1's red and yellow vectors, respectively, except now only one vector is shown for every 5 pixels (or 18.″5). Blue and green circles indicate locations of Class I and II YSOs, respectively, as identified by Zhang et al. (2019). The green beam in the bottom right shows the 18.″2 resolution of SOFIA observations. Bottom panel: LIC map overlaid on a column density map, where the wavy pattern indicates direction of the field. The LIC map filters out pixels for SNR less than 1.5 for P frac and 10 for Stokes I. For both panels, the beams on the right bottom and top are the FWHM resolution for SOFIA and Herschel spine/N gas maps, respectively.
Paper: The Magnetic Field in the Milky Way Filamentary Bone G47
Authors: Ian W. Stephens, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Cara Battersby, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara G.S. Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Simon Coudé, Andrés Guzmán, Alyssa Goodman, Takayoshi Kusune, Fábio P. Santos, Leah Zuckerman, Frankie Encalada
Figure caption: Results of the sliding box analysis, where a 74″ × 55.″5 rectangle was slid across the spine and the B-field was calculated via the DCFST technique. The size of the sliding rectangular box is shown toward the bottom left, with an example of a rectangular box rotated to be along the spine shown at the center of the image. Background for both images are Herschel 250 μm with the same stretch (colorbar) and beams as Figure 1. The left and right panels show the average B pos and λ within the sliding box, respectively. Black circles are locations where we were unable to calculate the field strengths.
Paper: The Magnetic Field in the Milky Way Filamentary Bone G47
Authors: Ian W. Stephens, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Cara Battersby, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara G.S. Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Simon Coudé, Andrés Guzmán, Alyssa Goodman, Takayoshi Kusune, Fábio P. Santos, Leah Zuckerman, Frankie Encalada
Figure caption: Plot of the plane of sky B-field (top panel) and the critical parameter, λ, (bottom panel) vs. the gas column density for each position along the spine for the sliding box analysis. Points are only shown for boxes with σ  θ  < 25°. Red and black points are for boxes where most the pixels within the box use a velocity dispersion based on 13CO and NH3(1,1) data sets, respectively. The dashed line is drawn at λ = 1; values higher than 1 are magnetically supercritical gas, where the B-field is weak enough to allow gravitational contraction.
Paper: The Magnetic Field in the Milky Way Filamentary Bone G47
Authors: Ian W. Stephens, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Cara Battersby, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara G.S. Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Simon Coudé, Andrés Guzmán, Alyssa Goodman, Takayoshi Kusune, Fábio P. Santos, Leah Zuckerman, Frankie Encalada
Figure caption: Histogram of B-field angle pixels at locations where N gas > 8 × 1021 cm−2. The vertical red line indicates the inferred average B-field angle of −23° across G47, which is based on summing Stokes Q and U with the same column density cutoff.
Paper: The Magnetic Field in the Milky Way Filamentary Bone G47
Authors: Ian W. Stephens, Philip C. Myers, Catherine Zucker, James M. Jackson, B.-G. Andersson, Rowan Smith, Archana Soam, Cara Battersby, Patricio Sanhueza, Taylor Hogge, Howard A. Smith, Giles Novak, Sarah Sadavoy, Thushara G.S. Pillai, Zhi-Yun Li, Leslie W. Looney, Koji Sugitani, Simon Coudé, Andrés Guzmán, Alyssa Goodman, Takayoshi Kusune, Fábio P. Santos, Leah Zuckerman, Frankie Encalada
Figure caption: Graphic illustrating how to calculate the magnetic flux for the sliding rectangular box technique.
Paper: Optical Rebrightening of Extragalactic Transients from the Zwicky Transient Facility
Authors: Monika Soraisam, Thomas Matheson, Chien-Hsiu Lee, Abhijit Saha, Gautham Narayan, Nicholas Wolf, Adam Scott, Stephanie Figuereo, Rafael Nuñez, Kevin McKinnon, Puragra Guhathakurta, Thomas G. Brink, Alexei V. Filippenko, Nathan Smith
Figure caption: Late-time spectra of bumpy extragalactic transients obtained using the Kast double-beam spectrograph on the Shane 3 m telescope at Lick Observatory. The epoch of the individual spectrum with respect to its first detection by ZTF is shown in the legend. The dip toward the red end (around 7800 Å) at epoch +803 d for SN 2019meh is due to imperfect cosmic-ray removal.
Paper: Optical Rebrightening of Extragalactic Transients from the Zwicky Transient Facility
Authors: Monika Soraisam, Thomas Matheson, Chien-Hsiu Lee, Abhijit Saha, Gautham Narayan, Nicholas Wolf, Adam Scott, Stephanie Figuereo, Rafael Nuñez, Kevin McKinnon, Puragra Guhathakurta, Thomas G. Brink, Alexei V. Filippenko, Nathan Smith
Figure caption: ZTF light curves of bumpy extragalactic transients. The lines and symbols are the same as in Figure 1. The top two panels (ZTF19aceqlxc/2019smj, ZTF20acklcyp/2020xkx) are SNe of Type IIn (Fremling et al. 2019; Gromadzki et al. 2020). ZTF19abclykm/2019meh is a Type II SLSN (Nicholl et al. 2019), and ZTF20aadchdd/2020cd an SN II (Dahiwale & Fremling 2020a). ZTF21aagppzg/2021blu is an LBV in the Spider galaxy (Uno et al. 2021), and ZTF21aanvncv/2021efd an SN Ib/c (Reguitti & Stritzinger 2021). Both ZTF20abisysx/2020nov (Dahiwale & Fremling 2020b) and ZTF20acwytxn/2020acka (Hammerstein et al. 2021) have been typed as TDEs, while 2020aeuh is an SNIa (Weil et al. 2021).
Paper: Optical Rebrightening of Extragalactic Transients from the Zwicky Transient Facility
Authors: Monika Soraisam, Thomas Matheson, Chien-Hsiu Lee, Abhijit Saha, Gautham Narayan, Nicholas Wolf, Adam Scott, Stephanie Figuereo, Rafael Nuñez, Kevin McKinnon, Puragra Guhathakurta, Thomas G. Brink, Alexei V. Filippenko, Nathan Smith
Figure caption: Example smoothed ZTF light curves. The five loci were chosen to highlight the quality of the celerite GP regression, which is represented by the solid lines. The green and red shaded regions show the 1σ uncertainty of the regression for the ZTF g and r passbands, respectively. The top two panels (ZTF18acvvudh, ZTF20acihinn) are SN candidates. In the middle panels, ZTF19abfqmjg is a nuclear transient candidate, while ZTF20aceeeuz has been classified as a nova in M33 (Reguitti 2020). The bottom panel is a Galactic dwarf nova (Watson et al. 2006). As is evident from the plots, the GP regression performs well for the extragalactic events, but fails for the dwarf nova.
Paper: Optical Rebrightening of Extragalactic Transients from the Zwicky Transient Facility
Authors: Monika Soraisam, Thomas Matheson, Chien-Hsiu Lee, Abhijit Saha, Gautham Narayan, Nicholas Wolf, Adam Scott, Stephanie Figuereo, Rafael Nuñez, Kevin McKinnon, Puragra Guhathakurta, Thomas G. Brink, Alexei V. Filippenko, Nathan Smith
Figure caption: Variation of the prominence of the peaks, Δm, against their corresponding widths, τ, for the final sample of loci. The green and red points indicate the results for the ZTF g and r passbands, respectively, while the background shading shows the density of these points (brighter regions have higher density values).
Paper: Prospects for Water Vapor Detection in the Atmospheres of Temperate and Arid Rocky Exoplanets around M-dwarf Stars
Authors: Feng Ding, and Robin D. Wordsworth
Figure caption: Schematic representation of the multiple moist-climate equilibrium states on synchronously rotating arid planets when the surface water is trapped by the substellar tropopause as a substellar oasis (a), entirely evaporated into the atmosphere in a post-runaway greenhouse climate state (b), and is trapped by the night-side surface as ice caps (c). The vertical axis represents the cold-trapping strength between the night-side surface and substellar tropopause. The hydrological cycle is dominated by the cold trap on the night-side surface when α ≪ 1 and at the substellar tropopause when α ≫ 1.
Paper: Prospects for Water Vapor Detection in the Atmospheres of Temperate and Arid Rocky Exoplanets around M-dwarf Stars
Authors: Feng Ding, and Robin D. Wordsworth
Figure caption: (a) Simulated JWST/NIRSpec Prism transmission spectra of a synchronously rotating planet with the night-side ice deposits. The atmosphere is made of 1 bar N2 and 10 ppmv H2O. Nocc = 9 is the number of transits needed to detect water features at an S/N = 5. Red points with 1σ error bars represent the simulated spectra from 9 transits. (b) The individual molecular absorption features for N2 (gray dash) and H2O (blue solid).
Paper: Prospects for Water Vapor Detection in the Atmospheres of Temperate and Arid Rocky Exoplanets around M-dwarf Stars
Authors: Feng Ding, and Robin D. Wordsworth
Figure caption: Required number of transits to detect water vapor features in the transmission spectra as a function of surface partial pressure of N2 and H2O. The respective night-side surface ice temperatures in ice-vapor-phase equilibrium with atmospheric water vapor are labeled in the upper x-axis. The white dashed lines show the lifetime of surface ice deposits estimated by the diffusion-limited escape flux. The surface ice layer is assumed to be 1 km thick and cover 10% of the global surface area. The climate state used to calculate the transmission spectrum in Figure 2 is marked by the white dot.
Paper: Prospects for Water Vapor Detection in the Atmospheres of Temperate and Arid Rocky Exoplanets around M-dwarf Stars
Authors: Feng Ding, and Robin D. Wordsworth
Figure caption: Simulated JWST/NIRSpec Prism transmission spectra of a synchronously rotating planet with 10 bar CO2 (blue) and 0.1 bar CO2 (red). Nocc is the number of transits needed to detect CO2 features at an S/N = 5. For the 0.1 bar CO2 case, atmospheric CO2 can condense on the night side and form CO2 ice deposits as on present-day Mars. Both cases assume the clear-sky condition.
Paper: The Chaotic History of the Retrograde Multi-planet System in K2-290A Driven by Distant Stars
Authors: Sergio Best, and Cristobal Petrovich
Figure caption: Schematic depiction of the K2-290 system. The planets b and c are nearly coplanar with an orbital plane inclined by ∼124° relative to the equator of star A. The distant M-dwarfs B and C have projected distances of ∼100 and ∼2000 au, respectively, and we define their mutual inclination as iBC.
Paper: The Chaotic History of the Retrograde Multi-planet System in K2-290A Driven by Distant Stars
Authors: Sergio Best, and Cristobal Petrovich
Figure caption: Evolution of the inclination of the stellar spin axis (﹩{i}_{{\rm{s}}}={\cos }^{-1}[\hat{{\boldsymbol{s}}}\cdot \hat{{\boldsymbol{z}}}]﹩) and the stellar obliquity (﹩{i}_{\mathrm{bc},{\rm{s}}}={\cos }^{-1}[\hat{{\boldsymbol{s}}}\cdot {\hat{{\boldsymbol{j}}}}_{\mathrm{bc}}]﹩) for two examples using the fiducial values given in Figure 1 and final J2 = 10−5.6. Panel a shows the case with spin down of the host star from P0 = 2 days to its current value of 6.63 days, while panel (b) shows the same case without spin down. In panel (c), we show the ZKL cycles of the AB binary and observe that sudden and chaotic changes in the obliquities coincide with the instances when the eccentricity peaks are reached.