adsabs/AstroCLIMB huggingface dataset:
Paper: Highly Significant Detection of X-Ray Polarization from the Brightest Accreting Neutron Star Sco X-1
Authors: Fabio La Monaca, Alessandro Di Marco, Juri Poutanen, Matteo Bachetti, Sara Elisa Motta, Alessandro Papitto, Maura Pilia, Fei Xie, Stefano Bianchi, Anna Bobrikova, Enrico Costa, Wei Deng, Ming-Yu Ge, Giulia Illiano, Shu-Mei Jia, Henric Krawczynski, Eleonora Veronica Lai, Kuan Liu, Guglielmo Mastroserio, Fabio Muleri, John Rankin, Paolo Soffitta, Alexandra Veledina, Filippo Ambrosino, Melania Del Santo, Wei Chen, Javier A. Garcia, Philip Kaaret, Thomas D. Russell, Wen-Hao Wei, Shuang-Nan Zhang, Chao Zuo, Zaven Arzoumanian, Massimo Cocchi, Andrea Gnarini, Ruben Farinelli, Keith Gendreau, Francesco Ursini, Martin C. Weisskopf, Silvia Zane, Iván Agudo, Lucio A. Antonelli, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu
Figure caption: Color–color diagram from the NuSTAR data. The soft color is defined as the source count rate in the 6–10 keV band divided by the one in 3–6 keV, while the hard color is the ratio of the 10–20 keV count rate to the one in 6–10 keV. Gray points represent the past NuSTAR observations, while the colored ones report from blue to green the elapsed time since the start of the present NuSTAR observation simultaneous with IXPE.
Paper: Highly Significant Detection of X-Ray Polarization from the Brightest Accreting Neutron Star Sco X-1
Authors: Fabio La Monaca, Alessandro Di Marco, Juri Poutanen, Matteo Bachetti, Sara Elisa Motta, Alessandro Papitto, Maura Pilia, Fei Xie, Stefano Bianchi, Anna Bobrikova, Enrico Costa, Wei Deng, Ming-Yu Ge, Giulia Illiano, Shu-Mei Jia, Henric Krawczynski, Eleonora Veronica Lai, Kuan Liu, Guglielmo Mastroserio, Fabio Muleri, John Rankin, Paolo Soffitta, Alexandra Veledina, Filippo Ambrosino, Melania Del Santo, Wei Chen, Javier A. Garcia, Philip Kaaret, Thomas D. Russell, Wen-Hao Wei, Shuang-Nan Zhang, Chao Zuo, Zaven Arzoumanian, Massimo Cocchi, Andrea Gnarini, Ruben Farinelli, Keith Gendreau, Francesco Ursini, Martin C. Weisskopf, Silvia Zane, Iván Agudo, Lucio A. Antonelli, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu
Figure caption: Light curves from the simultaneous observations of Sco X-1, from top to bottom: IXPE (DU1, DU2, and DU3), NICER, NuSTAR (FPMA and FPMB), and Insight-HXMT. They show that all the observations are well overlapped with the IXPE one. The flaring activity of the source is seen in all the simultaneous observations (dark gray shaded regions), while the nonflaring periods are identified with the light gray bands.
Paper: Highly Significant Detection of X-Ray Polarization from the Brightest Accreting Neutron Star Sco X-1
Authors: Fabio La Monaca, Alessandro Di Marco, Juri Poutanen, Matteo Bachetti, Sara Elisa Motta, Alessandro Papitto, Maura Pilia, Fei Xie, Stefano Bianchi, Anna Bobrikova, Enrico Costa, Wei Deng, Ming-Yu Ge, Giulia Illiano, Shu-Mei Jia, Henric Krawczynski, Eleonora Veronica Lai, Kuan Liu, Guglielmo Mastroserio, Fabio Muleri, John Rankin, Paolo Soffitta, Alexandra Veledina, Filippo Ambrosino, Melania Del Santo, Wei Chen, Javier A. Garcia, Philip Kaaret, Thomas D. Russell, Wen-Hao Wei, Shuang-Nan Zhang, Chao Zuo, Zaven Arzoumanian, Massimo Cocchi, Andrea Gnarini, Ruben Farinelli, Keith Gendreau, Francesco Ursini, Martin C. Weisskopf, Silvia Zane, Iván Agudo, Lucio A. Antonelli, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu
Figure caption: Polar plot of the X-ray polarization for Sco X-1 in the two different flaring (dark gray) and nonflaring (light gray) states; the two states show a compatible polarization. The contours are at 90% CL.
Paper: Highly Significant Detection of X-Ray Polarization from the Brightest Accreting Neutron Star Sco X-1
Authors: Fabio La Monaca, Alessandro Di Marco, Juri Poutanen, Matteo Bachetti, Sara Elisa Motta, Alessandro Papitto, Maura Pilia, Fei Xie, Stefano Bianchi, Anna Bobrikova, Enrico Costa, Wei Deng, Ming-Yu Ge, Giulia Illiano, Shu-Mei Jia, Henric Krawczynski, Eleonora Veronica Lai, Kuan Liu, Guglielmo Mastroserio, Fabio Muleri, John Rankin, Paolo Soffitta, Alexandra Veledina, Filippo Ambrosino, Melania Del Santo, Wei Chen, Javier A. Garcia, Philip Kaaret, Thomas D. Russell, Wen-Hao Wei, Shuang-Nan Zhang, Chao Zuo, Zaven Arzoumanian, Massimo Cocchi, Andrea Gnarini, Ruben Farinelli, Keith Gendreau, Francesco Ursini, Martin C. Weisskopf, Silvia Zane, Iván Agudo, Lucio A. Antonelli, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu
Figure caption: Spectral joint fit of the Stokes parameters I, Q, and U in EF E  representation in the 2–8 keV energy band using the three IXPE detectors and applying the model tbabs*(gauss+polconst*diskbb+polconst*nthcomp). The best fit has χ 2/dof = 1329/1337 = 0.99. Energy rebinning is only for plotting purposes.
Paper: Highly Significant Detection of X-Ray Polarization from the Brightest Accreting Neutron Star Sco X-1
Authors: Fabio La Monaca, Alessandro Di Marco, Juri Poutanen, Matteo Bachetti, Sara Elisa Motta, Alessandro Papitto, Maura Pilia, Fei Xie, Stefano Bianchi, Anna Bobrikova, Enrico Costa, Wei Deng, Ming-Yu Ge, Giulia Illiano, Shu-Mei Jia, Henric Krawczynski, Eleonora Veronica Lai, Kuan Liu, Guglielmo Mastroserio, Fabio Muleri, John Rankin, Paolo Soffitta, Alexandra Veledina, Filippo Ambrosino, Melania Del Santo, Wei Chen, Javier A. Garcia, Philip Kaaret, Thomas D. Russell, Wen-Hao Wei, Shuang-Nan Zhang, Chao Zuo, Zaven Arzoumanian, Massimo Cocchi, Andrea Gnarini, Ruben Farinelli, Keith Gendreau, Francesco Ursini, Martin C. Weisskopf, Silvia Zane, Iván Agudo, Lucio A. Antonelli, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, Chi-Yung Ng, Stephen L. O'Dell, Nicola Omodei, Chiara Oppedisano, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu
Figure caption: Spectral energy distribution of Sco X-1 in EF E  representation. The points show the data from NICER (brown), NuSTAR (blue), Insight-HXMT (green), and IXPE (red). The different spectral model components are reported with black lines for diskbb (long-dashed), nthcomp (dotted), and gauss (short-dashed). The bottom panel shows the residuals between the data and the best-fit model A.
Paper: First Detection of an Overmassive Black Hole Galaxy UHZ1: Evidence for Heavy Black Hole Seed Formation from Direct Collapse
Authors: Priyamvada Natarajan, Fabio Pacucci, Angelo Ricarte, Ákos Bogdán, Andy D. Goulding, Nico Cappelluti
Figure caption: Schematic diagram of the potential assembly history of the OBG candidate UHZ1. The direct collapse of primordial gas disks resulting in the production of heavy initial black hole seeds has been demonstrated to occur feasibly in the setting shown here: satellite DCBH halos that are bound to parent star-forming halos (see Figure 1 in Natarajan et al. 2017). Star formation in the satellite atomic cooling DCBH halo is expected to be suppressed due to the dissociation of molecular hydrogen from the Lyman–Werner radiation produced by the parent galaxy. As a consequence, the OBG is a merger remnant that contains a growing DCBH seed with an initial mass of ∼104 M ⊙ with M bh ≥ M *.
Paper: First Detection of an Overmassive Black Hole Galaxy UHZ1: Evidence for Heavy Black Hole Seed Formation from Direct Collapse
Authors: Priyamvada Natarajan, Fabio Pacucci, Angelo Ricarte, Ákos Bogdán, Andy D. Goulding, Nico Cappelluti
Figure caption: The OBG model match for UHZ1: the model spectrum overplotted here is obtained by growing an initially heavy seed of ∼104 M ⊙ to a final mass of 107 M ⊙ as estimated for UHZ1 and combining with a young stellar population (age of 350 Myr), low metallicity (﹩{10}^{-3}\,{Z}_{{M}_{\odot }}﹩) with a column density of ∼3 × 1024 cm−2. The observed near-IR JWST SED for UHZ1 points taken from Castellano et al. (2023) are shown in blue. We note that the overplotted SED template from our library generated with the parameters noted above is very similar to UHZ1.
Paper: First Detection of an Overmassive Black Hole Galaxy UHZ1: Evidence for Heavy Black Hole Seed Formation from Direct Collapse
Authors: Priyamvada Natarajan, Fabio Pacucci, Angelo Ricarte, Ákos Bogdán, Andy D. Goulding, Nico Cappelluti
Figure caption: The template match for the multiwavelength SED from our library of OBG models on which we overplot the measured fluxes in the IR from JWST and X-ray from Chandra for UHZ1 shows that they are consistent and well matched. The template that provides this optimal match has the following properties: a heavy initial seed with a mass of 104 M ⊙; the OBG accreting at the Eddington limit with an age of 350 Myr for the recently merged stellar population with a low metallicity of ∼10−3 Z ⊙ and a column density of 3 × 1024 cm−2, shown in Figure 2 (in red).
Paper: First Detection of an Overmassive Black Hole Galaxy UHZ1: Evidence for Heavy Black Hole Seed Formation from Direct Collapse
Authors: Priyamvada Natarajan, Fabio Pacucci, Angelo Ricarte, Ákos Bogdán, Andy D. Goulding, Nico Cappelluti
Figure caption: Selection criteria for OBGs: the predicted location of OBGs in color–color space, with the location of UHZ1 marked with a black star.
Paper: Tidal Disruption of Near-Earth Asteroids during Close Encounters with Terrestrial Planets
Authors: Mikael Granvik, Kevin J. Walsh
Figure caption: The difference (blue line) between the observed and predicted number of NEO detections by CSS during the years 2005–2012 as a function of eccentricity e (top panels) and inclination i (bottom panels) for perihelion distances coinciding with the semimajor axis of Venus (left panels) and the semimajor axis of Earth (right panels). The model prediction assumes a super-catastrophic disruption when q ∼ 0.076  au (Granvik et al. 2016). The gray histograms show arbitrarily normalized distributions of e and i of synthetic gravitational aggregates that in numerical simulations have undergone B-type tidal disruptions during encounters with Earth or Venus.
Paper: Tidal Disruption of Near-Earth Asteroids during Close Encounters with Terrestrial Planets
Authors: Mikael Granvik, Kevin J. Walsh
Figure caption: The difference between observed and predicted number of NEO detections by CSS during the years 2005–2012 as a function of perihelion distance q (blue line). The model prediction assumes a super-catastrophic disruption when q ∼ 0.076  au (Granvik et al. 2016). The observed population is substantially larger than the predicted population for q ∼ a Venus ∼ 0.7  au and q ∼ a Earth ∼ 1  au. The difference cannot be explained by selection effects or orbital dynamics. The gray histogram shows an arbitrarily normalized distribution of the perihelion distances of synthetic gravitational aggregates that in numerical simulations have undergone B-type tidal disruptions during encounters with Earth or Venus.
Paper: Tidal Disruption of Near-Earth Asteroids during Close Encounters with Terrestrial Planets
Authors: Mikael Granvik, Kevin J. Walsh
Figure caption: Examples of ensemble orbit distributions that could result from a large number of tidal disruptions of NEOs with a < 2  au and i < 25° during close encounters with Earth 10 kyr after the disruption (left) and when all test asteroids have reached a sink (right). The assumption here is that the fragments are ejected at negligibly slow speeds relative to the disrupting parent body, which is corroborated by numerical simulations of tidal disruptions (Schunová et al. 2014), so only the orbital evolutions of the parent bodies are considered here.
Paper: Tidal Disruption of Near-Earth Asteroids during Close Encounters with Terrestrial Planets
Authors: Mikael Granvik, Kevin J. Walsh
Figure caption: The difference between the observed and predicted number of NEO detections by CSS during the years 2005–2012 as a function of perihelion distance q separated into four different ranges in absolute magnitude H. The model prediction assumes a super-catastrophic disruption when q ∼ 0.076  au (Granvik et al. 2016). The excess detections at q ∼ 0.7  au and q ∼ 1  au correspond, in general, to smaller NEOs. See the main text for caveats affecting interpretation.
Paper: Tidal Disruption of Near-Earth Asteroids during Close Encounters with Terrestrial Planets
Authors: Mikael Granvik, Kevin J. Walsh
Figure caption: The difference between observed and predicted number of NEO detections by CSS during the years 2005–2012 as a function of perihelion distance q when including orbit distributions that could result from tidal disruptions in the model (blue line). The model accounts for super-catastrophic disruptions by fitting for the parameters of a penalty function at small q (Granvik et al. 2018). The gray histogram is the one not accounting for tidal disruptions (Figure 1).
Paper: Three-dimensional GRMHD Simulations of Neutron Star Jets
Authors: Pushpita Das, Oliver Porth
Figure caption: Stellar and disk magnetic field interaction for χ star = 0° (left) and 90° (right). The upper panels show the initial magnetic field, and the lower panels show the interaction at an intermediate time. The blue and red lines in the lower panel show the field lines in the upper and lower jet, respectively. The magnetic reconnection of field lines with opposing polarity is indicated by the purple and green boxes. The purple boxes represent the reconnection of the initially closed stellar zone, while the green boxes represent the reconnection of the initially open stellar field lines. The dotted lines in panel (c) represent the newly open field lines as a result of reconnection of the stellar closed zone. The dashed lines in panel (d) show how the initially open field lines in the lower right and upper left get rearranged by the disk due to magnetic reconnection. The accretion column has a shifted position as a consequence of the rearrangement of the polar field lines.
Paper: Three-dimensional GRMHD Simulations of Neutron Star Jets
Authors: Pushpita Das, Oliver Porth
Figure caption: Surface maps of the open magnetic field lines powering the jet for different stellar magnetic axis inclinations in the accreting regime. The blue and red colors represent the field lines ending up in the jet in the northern (z > 0) and southern (z < 0) hemispheres, respectively. The first column (a) represents the magnetic footpoints of the open field lines at an initial time (mimicking the isolated case), and the second column (b) shows the footpoints of the open field lines in the jet at a later time (after reaching the quasi-stationary state). The green arrow indicates the direction of the magnetic moment. For a dipolar geometry, the polarity of the magnetic field flips at the magnetic equator (outlined by the green circle), b  r  > 0 (outgoing field lines) in the hemisphere along the magnetic moment and b  r  < 0 (ingoing field lines) in the rest of the hemisphere.
Paper: Three-dimensional GRMHD Simulations of Neutron Star Jets
Authors: Pushpita Das, Oliver Porth
Figure caption: Variation of jet power (a) and open flux (b) with magnetic axis inclination (χ star). The vertical axis shows the mean quantities normalized by the aligned isolated cases for t ∈ [15,000, 25,000]r  g /c. The red dashed lines represent the variation of power and open flux in the isolated cases. The values of isolated open flux as a function of χ star are adopted from Tchekhovskoy et al. (2013).
Paper: Three-dimensional GRMHD Simulations of Neutron Star Jets
Authors: Pushpita Das, Oliver Porth
Figure caption:  θ profiles of different quantities for χ star = 0° (blue) and 90° (red). Panel (a) shows the time evolution of the quantities at the stellar surface. Panels (b) and (c) show the time evolution at 50rg  in the regions with σ > 1. The dotted and dotted–dashed lines in (a) show ﹩\langle {{B}^{r}}^{2}{\rangle }_{\phi }﹩ at t ∈ [0, 20,000]r  g /c. The solid and dashed lines in panels (b) and (c) show ﹩\langle {{B}^{r}}^{2}{\rangle }_{\phi }﹩ at t = t 0 and ﹩\langle {T}_{{\rm{t}},\mathrm{EM}}^{r}{\rangle }_{\phi }﹩, respectively. Here t 0 = 200r  g /c (b) and t 0 = 20,000r  g /c (c).
Paper: Three-dimensional GRMHD Simulations of Neutron Star Jets
Authors: Pushpita Das, Oliver Porth
Figure caption: Jet structure in the z–x plane for (a) an accreting case with χ star = 60°, μ = 20, and Ω = 0.03 and (b) a strong propeller with χ star = 60°, μ = 30, and Ω = 0.05. The color bar shows log10 σ, and the white lines show the σ = 1 contour. The gray dashed and solid lines show the corotation radius and light cylinder radius, respectively.
Paper: Three-dimensional GRMHD Simulations of Neutron Star Jets
Authors: Pushpita Das, Oliver Porth
Figure caption: Surface maps of the open magnetic field lines powering the jet in the upper (blue) and lower (red) hemispheres. Here χ star = 60°, μ = 30, and Ω = 0.05. The two panels show the surface maps at two different times: (a) early and (b) quasi-stationary state. All labels are the same as in Figure 4.
Paper: Three-dimensional GRMHD Simulations of Neutron Star Jets
Authors: Pushpita Das, Oliver Porth
Figure caption: (a) Mass accretion rate at the stellar surface for different stellar magnetic inclinations. (b) Evolution of jet power with time for different magnetic inclinations. The jet is defined as the σ = 1 contour. The mass accretion rate and jet power are extracted at 4.2r  g  and 50r  g , respectively.