adsabs/AstroCLIMB huggingface dataset:
Paper: Effects of Supra-arcade Downflows Interacting with the Postflare Arcade
Authors: Arun Kumar Awasthi, Rui Liu, Tingyu Gou
Figure caption: EUV overview of the SAD cases observed in the gradual phase of an M6.5 flare of 2013 April 11. (a) Disk-integrated X-ray intensity profile in 1–8 Å (black) and 0.5–4 Å (pink), depicting the prolonged gradual phase of the flare. Depression in EM values within SADs in the 7–12 MK temperature range is plotted in blue for all the SAD cases (scaled on the right y-axis; discussed in Section 3.1). (b) Full-disk view of the flaring region AR 11719 in 131 Å. An upright view of the flaring region, prepared by zooming in and rotating the field of view of the active region by 130° clockwise, is shown in the inset. In addition to the postflare loops, the bright supra-arcade region exhibiting various structures such as rays, dark lanes, and haze can be identified. Six cases of dark voids seen in the AIA 131 Å images (denoted by yellow arrows) are shown in the middle panels (c)–(h) while corresponding running-difference images are plotted in the bottom panels (i)–(n), respectively. Images are rotated clockwise with angles varying in the range 120°–135° to present the upright view of the descending voids. SAD cases #1–6 are annotated in panel (a) and also in the middle row.
Paper: Effects of Supra-arcade Downflows Interacting with the Postflare Arcade
Authors: Arun Kumar Awasthi, Rui Liu, Tingyu Gou
Figure caption: Thermal characteristics of three SADs as derived from the EUV observations. The first two rows present thermal properties of SAD case #1, observed at 07:39:37 UT, as observed in EUV wavelengths (94 and 131 Å, shown in (a) and (b)). Enhanced emission measure at 5–7 MK within the void is evident in the EM maps (3–5 MK, 5–7 MK, and 7–12 MK in panels (c)–(e)) as well as in the plot of EM values (f) in various temperature ranges along a horizontal (yellow) line drawn in panel (b) that slices the blob. The maximum value of uncertainty in the respective EM values is plotted as error bars on the right. (g) 94 Å (red) and 131 Å (blue) intensity profiles along the horizontal line slicing the blob deduced from the EUV images acquired at 07:39:37 UT (full) and 07:40:01 UT (dotted). “+” signs in EUV images and vertical lines in the plots mark the blob positions. Similarly, thermodynamical characteristics of SAD case #2 (07:50:13 UT; panels (h)–(k)) also reveal the enhanced EM values in the 5–7 MK temperature bin (EM map (i) and plot (k)). (l)–(o) On the other hand, thermal properties of SAD case #5 (at 08:17:25 UT), shown in the bottom panels, only exhibit depleted EM values at the location of the void in all the investigated temperature bins. The level of depression in EM values (R EM) at the SAD location is shown by a vertical double-headed arrow and annotated for SAD cases #1 (f), #2 (k), and #5 (o).
Paper: DUVET: Spatially Resolved Observations of Star Formation Regulation via Galactic Outflows in a Starbursting Disk Galaxy
Authors: Bronwyn Reichardt Chu, Deanne B. Fisher, Alberto D. Bolatto, John Chisholm, Drummond Fielding, Danielle Berg, Alex J. Cameron, Karl Glazebrook, Rodrigo Herrera-Camus, Glenn G. Kacprzak, Laura Lenkić, Miao Li, Daniel K. McPherson, Nikole M. Nielsen, Danail Obreschkow, Ryan J. Rickards Vaught, Karin Sandstrom
Figure caption: Ionized gas outflow mass flux (﹩{\dot{{\rm{\Sigma }}}}_{\mathrm{out}}﹩) compared to SFR surface density (ΣSFR) for ∼500 pc resolution pixels in IRAS08 where we have observed an outflow. The blue points are calculated assuming an n  e  normalized to 100 cm−3, and the faint gray points use an assumed n  e  = 300 cm−3. A typical error bar is shown in the top left corner. We fit a relationship to the two quantities, which returns a slightly nonlinear correlation. Yet, within the scatter, the data is also consistent with a linear correlation (within 1.5σ).
Paper: DUVET: Spatially Resolved Observations of Star Formation Regulation via Galactic Outflows in a Starbursting Disk Galaxy
Authors: Bronwyn Reichardt Chu, Deanne B. Fisher, Alberto D. Bolatto, John Chisholm, Drummond Fielding, Danielle Berg, Alex J. Cameron, Karl Glazebrook, Rodrigo Herrera-Camus, Glenn G. Kacprzak, Laura Lenkić, Miao Li, Daniel K. McPherson, Nikole M. Nielsen, Danail Obreschkow, Ryan J. Rickards Vaught, Karin Sandstrom
Figure caption: Maps of IRAS08. (Left) Map of Hα flux from HST. (Right) Mass-outflow flux, ﹩{\dot{{\rm{\Sigma }}}}_{\mathrm{out}}﹩, found in each spaxel using [O III] λ5007 and Hβ emission line flux from observations with KCWI on board Keck II (RC22). Only spaxels where an outflow was detected are included. The ﹩{\dot{{\rm{\Sigma }}}}_{\mathrm{out}}﹩ values were scaled to assume electron densities of n  e  = 100 cm−3. Outflowing gas driven by star formation has been resolved across the disk of IRAS08.
Paper: Magnetohydrodynamic Model of Late Accretion onto a Protoplanetary Disk: Cloudlet Encounter Event
Authors: Masaki Unno, Tomoyuki Hanawa, Shinsuke Takasao
Figure caption: Time evolution of the surface density distribution. Reddish lines show the results of the model with a  s  = 75 au, while bluish lines show the model with a  s  = 100 au.
Paper: Magnetohydrodynamic Model of Late Accretion onto a Protoplanetary Disk: Cloudlet Encounter Event
Authors: Masaki Unno, Tomoyuki Hanawa, Shinsuke Takasao
Figure caption: Phase diagram under different conditions of cloudlet size (a  z ) and magnetic field strength (B 0) at t = 9008 yr. White arrows indicate spirals.
Paper: Magnetohydrodynamic Model of Late Accretion onto a Protoplanetary Disk: Cloudlet Encounter Event
Authors: Masaki Unno, Tomoyuki Hanawa, Shinsuke Takasao
Figure caption: Same as Figure 9, but for S60_B116 and S150_B116 with fixed boundary conditions (S60_B116_Fix and S150_B116_Fix) and outgoing boundary conditions (S60_B116_Outgo and S150_B116_Outgo). The vertical ranges of the two panels are different.
Paper: Magnetohydrodynamic Model of Late Accretion onto a Protoplanetary Disk: Cloudlet Encounter Event
Authors: Masaki Unno, Tomoyuki Hanawa, Shinsuke Takasao
Figure caption: 3D structure of S60_B116 (left) and S150_B116 (right) with outgoing boundary conditions at t = 3378 yr.
Paper: Magnetohydrodynamic Model of Late Accretion onto a Protoplanetary Disk: Cloudlet Encounter Event
Authors: Masaki Unno, Tomoyuki Hanawa, Shinsuke Takasao
Figure caption: Same as Figure 9, but for S60_B116 and S150_B116 with a s = 75,  100 au.
Paper: Magnetohydrodynamic Model of Late Accretion onto a Protoplanetary Disk: Cloudlet Encounter Event
Authors: Masaki Unno, Tomoyuki Hanawa, Shinsuke Takasao
Figure caption: 3D structure of S60_B116 (left) and S150_B116 (right) with a s = 75 au at t = 3378 yr.
Paper: DUVET: Spatially Resolved Observations of Star Formation Regulation via Galactic Outflows in a Starbursting Disk Galaxy
Authors: Bronwyn Reichardt Chu, Deanne B. Fisher, Alberto D. Bolatto, John Chisholm, Drummond Fielding, Danielle Berg, Alex J. Cameron, Karl Glazebrook, Rodrigo Herrera-Camus, Glenn G. Kacprzak, Laura Lenkić, Miao Li, Daniel K. McPherson, Nikole M. Nielsen, Danail Obreschkow, Ryan J. Rickards Vaught, Karin Sandstrom
Figure caption: The outflow efficiency ﹩{\dot{{\rm{\Sigma }}}}_{\mathrm{out}}/{{\rm{\Sigma }}}_{\mathrm{mol}}﹩ of IRAS08 plotted against the star formation efficiency ΣSFR/Σmol (left), and SFR surface density ΣSFR (right). In both panels, the blue circles represent our IRAS08 data using n  e  = 100 cm−3. Fainter gray circles represent IRAS08 if an electron density of n  e  = 300 cm−3 were used. A typical error bar is shown in the top left corner. M82, the central kiloparsec of NGC 1482, and the center of NGC 253 are denoted by the black diamond, green triangle, and dark red square, respectively. Open symbols for these galaxies indicate the results for the molecular gas mass-outflow rate, and filled-in symbols indicate the ionized gas mass-outflow rate. In the left panel, the 1:1 and 10:1 ratios of the outflow efficiency to star formation efficiency are plotted as gray dashed lines. A fit to the IRAS08 data is given by the solid black line. In the right panel, the solid black line shows a fit of the outflow efficiency to ΣSFR. In high ΣSFR regions, IRAS08 drives more efficient outflows.
Paper: DUVET: Spatially Resolved Observations of Star Formation Regulation via Galactic Outflows in a Starbursting Disk Galaxy
Authors: Bronwyn Reichardt Chu, Deanne B. Fisher, Alberto D. Bolatto, John Chisholm, Drummond Fielding, Danielle Berg, Alex J. Cameron, Karl Glazebrook, Rodrigo Herrera-Camus, Glenn G. Kacprzak, Laura Lenkić, Miao Li, Daniel K. McPherson, Nikole M. Nielsen, Danail Obreschkow, Ryan J. Rickards Vaught, Karin Sandstrom
Figure caption: The mass-loading factor of ionized gas, η ion, as a function of the molecular gas surface density, Σmol (left panel) and the SFR surface density, ΣSFR (right panel). Observational data from IRAS08 is given in circles colored by outflow efficiency using n  e  = 100 cm−1, with rescaled values for an electron density of n  e  = 300 cm−1 as open circles. The black arrows show the magnitude and direction the median η ion value would move if we assumed an outflow extent of R out = 0.1R vir (open arrow represents the median with n  e  = 300 cm−1). Typical error bars for the IRAS08 data are shown in the top right corner of each panel. We compare our observational results from IRAS08 with results from the FIRE-2 (Pandya et al. 2021, Figure 11) and TIGRESS (Kim et al. 2020, Figure 9) simulations. Results from the warm-phase gas (103 < T < 105 K) from FIRE-2 are shown as gray squares. The Σmol–η ion and ΣSFR–η ion relationships found in Kim et al. (2020) for the cool gas component (T < 2 × 104 K) are plotted with solid black lines, and extrapolated past the parameter space they covered with the dashed black lines. The simulation data is not inconsistent with our observational results.
Paper: DUVET: Spatially Resolved Observations of Star Formation Regulation via Galactic Outflows in a Starbursting Disk Galaxy
Authors: Bronwyn Reichardt Chu, Deanne B. Fisher, Alberto D. Bolatto, John Chisholm, Drummond Fielding, Danielle Berg, Alex J. Cameron, Karl Glazebrook, Rodrigo Herrera-Camus, Glenn G. Kacprzak, Laura Lenkić, Miao Li, Daniel K. McPherson, Nikole M. Nielsen, Danail Obreschkow, Ryan J. Rickards Vaught, Karin Sandstrom
Figure caption: The resolved relationship between SFR surface density, ΣSFR, and molecular gas surface density, Σmol. The circles of IRAS08 are colored according to the mass-outflow flux, ﹩{\dot{{\rm{\Sigma }}}}_{\mathrm{out}}﹩. Note that the vertical blue line denotes the largest of the ΣSFR error bars, and the rest of the error bars are smaller than the points. A typical error bar is shown in the top left corner. The gray points represent data from the HERACLES sample of local spirals (Leroy et al. 2013). NGC253 (Bolatto et al. 2013a), M82 (Leroy et al. 2015b), and NGC1482 (Veilleux & Rupke 2002; Salak et al. 2020) are represented as a dark red square, a black diamond, and a green triangle, respectively. The dashed lines indicate where the time it takes to deplete the molecular gas through star formation, t dep,SF, would be 0.1 Gyr (top line) and 1.0 Gyr (bottom line). In IRAS08, a greater distance from the spiral sequence (gray points) in ΣSFR−Σmol corresponds to outflows with higher mass-outflow rates and higher momentum flux.
Paper: DUVET: Spatially Resolved Observations of Star Formation Regulation via Galactic Outflows in a Starbursting Disk Galaxy
Authors: Bronwyn Reichardt Chu, Deanne B. Fisher, Alberto D. Bolatto, John Chisholm, Drummond Fielding, Danielle Berg, Alex J. Cameron, Karl Glazebrook, Rodrigo Herrera-Camus, Glenn G. Kacprzak, Laura Lenkić, Miao Li, Daniel K. McPherson, Nikole M. Nielsen, Danail Obreschkow, Ryan J. Rickards Vaught, Karin Sandstrom
Figure caption: The gas fraction, f gas ≡ Σmol/(Σmol + Σstar), is compared to the orbital frequency, Ω. Data points for IRAS08 are colored by the outflow momentum flux, dp/dt. A typical error bar for the IRAS08 data is shown in the bottom left corner. The dashed line shows the boundary predicted by Orr et al. (2022a) between outflows that breakout of the disk, and outflows that are stalled within the disk (see their Figures 1 and 2). Gray squares indicate resolved observations of local spiral galaxies with no observed outflow. Red squares indicate the resolved observations of the outflow in NGC 253. We find that ∼85% of our resolved regions are within the predicted region for breakout outflows.
Paper: EMPRESS. VIII. A New Determination of Primordial He Abundance with Extremely Metal-poor Galaxies: A Suggestion of the Lepton Asymmetry and Implications for the Hubble Tension
Authors: Akinori Matsumoto, Masami Ouchi, Kimihiko Nakajima, Masahiro Kawasaki, Kai Murai, Kentaro Motohara, Yuichi Harikane, Yoshiaki Ono, Kosuke Kushibiki, Shuhei Koyama, Shohei Aoyama, Masahiro Konishi, Hidenori Takahashi, Yuki Isobe, Hiroya Umeda, Yuma Sugahara, Masato Onodera, Kentaro Nagamine, Haruka Kusakabe, Yutaka Hirai, Takashi J. Moriya, Takatoshi Shibuya, Yutaka Komiyama, Keita Fukushima, Seiji Fujimoto, Takashi Hattori, Kohei Hayashi, Akio K. Inoue, Shotaro Kikuchihara, Takashi Kojima, Yusei Koyama, Chien-Hsiu Lee, Ken Mawatari, Takashi Miyata, Tohru Nagao, Shinobu Ozaki, Michael Rauch, Tomoki Saito, Akihiro Suzuki, Tsutomu T. Takeuchi, Masayuki Umemura, Yi Xu, Kiyoto Yabe, Yechi Zhang, Yuzuru Yoshii
Figure caption: Rest-frame spectra of Subaru galaxies, taken with IRCS, SWIMS, and MOIRCS. The blue lines and red lines present the fluxes and the 1σ errors, respectively. Note that the emission lines of the IRCS spectra have profiles similar to box shapes due to the spatially extended objects observed with a large slit width for IRCS, while this does not affect the flux measurements by summing the pixels above the continuum.
Paper: DUVET: Spatially Resolved Observations of Star Formation Regulation via Galactic Outflows in a Starbursting Disk Galaxy
Authors: Bronwyn Reichardt Chu, Deanne B. Fisher, Alberto D. Bolatto, John Chisholm, Drummond Fielding, Danielle Berg, Alex J. Cameron, Karl Glazebrook, Rodrigo Herrera-Camus, Glenn G. Kacprzak, Laura Lenkić, Miao Li, Daniel K. McPherson, Nikole M. Nielsen, Danail Obreschkow, Ryan J. Rickards Vaught, Karin Sandstrom
Figure caption: The combined ﹩{{\rm{\Sigma }}}_{\mathrm{SFR}}+{\dot{{\rm{\Sigma }}}}_{\mathrm{out}}﹩ is compared to Σmol for regions in IRAS08, and shown as the solid points. Colors indicate the fraction of the total SFR in the corresponding area. A typical error bar is shown in the top left corner. The combined SFR and outflow mass flux represent a more complete view of gas removal. Open symbols represent only ΣSFR, for comparison. In lower ΣSFR regions the combination only makes a factor ∼2 change to the gas depletion time (dashed lines), but at high ΣSFR it decreases the total depletion time by nearly an order of magnitude.
Paper: EMPRESS. VIII. A New Determination of Primordial He Abundance with Extremely Metal-poor Galaxies: A Suggestion of the Lepton Asymmetry and Implications for the Hubble Tension
Authors: Akinori Matsumoto, Masami Ouchi, Kimihiko Nakajima, Masahiro Kawasaki, Kai Murai, Kentaro Motohara, Yuichi Harikane, Yoshiaki Ono, Kosuke Kushibiki, Shuhei Koyama, Shohei Aoyama, Masahiro Konishi, Hidenori Takahashi, Yuki Isobe, Hiroya Umeda, Yuma Sugahara, Masato Onodera, Kentaro Nagamine, Haruka Kusakabe, Yutaka Hirai, Takashi J. Moriya, Takatoshi Shibuya, Yutaka Komiyama, Keita Fukushima, Seiji Fujimoto, Takashi Hattori, Kohei Hayashi, Akio K. Inoue, Shotaro Kikuchihara, Takashi Kojima, Yusei Koyama, Chien-Hsiu Lee, Ken Mawatari, Takashi Miyata, Tohru Nagao, Shinobu Ozaki, Michael Rauch, Tomoki Saito, Akihiro Suzuki, Tsutomu T. Takeuchi, Masayuki Umemura, Yi Xu, Kiyoto Yabe, Yechi Zhang, Yuzuru Yoshii
Figure caption: Histograms showing the distributions of the best-recovered values of y +,  a He,  τ He,  c(Hβ), and a H for the mock “observed” flux sets in cases (X) (top panels) and (Y) (bottom panels). The solid red lines represent the “true” values of the parameters.
Paper: EMPRESS. VIII. A New Determination of Primordial He Abundance with Extremely Metal-poor Galaxies: A Suggestion of the Lepton Asymmetry and Implications for the Hubble Tension
Authors: Akinori Matsumoto, Masami Ouchi, Kimihiko Nakajima, Masahiro Kawasaki, Kai Murai, Kentaro Motohara, Yuichi Harikane, Yoshiaki Ono, Kosuke Kushibiki, Shuhei Koyama, Shohei Aoyama, Masahiro Konishi, Hidenori Takahashi, Yuki Isobe, Hiroya Umeda, Yuma Sugahara, Masato Onodera, Kentaro Nagamine, Haruka Kusakabe, Yutaka Hirai, Takashi J. Moriya, Takatoshi Shibuya, Yutaka Komiyama, Keita Fukushima, Seiji Fujimoto, Takashi Hattori, Kohei Hayashi, Akio K. Inoue, Shotaro Kikuchihara, Takashi Kojima, Yusei Koyama, Chien-Hsiu Lee, Ken Mawatari, Takashi Miyata, Tohru Nagao, Shinobu Ozaki, Michael Rauch, Tomoki Saito, Akihiro Suzuki, Tsutomu T. Takeuchi, Masayuki Umemura, Yi Xu, Kiyoto Yabe, Yechi Zhang, Yuzuru Yoshii
Figure caption: Probability distribution functions (PDFs) of model parameters of J1201+0211 recovered with YMCMC (Hsyu et al. 2020). One-dimensional PDFs are shown in the diagonal panels, and two-dimensional PDFs are shown in the off-diagonal panels with contours showing the 1σ, 2σ, and 3σ levels. The red solid lines represent the best-recovered parameter value, and the black dashed lines represents the 68% confidence range for each parameter. In the panels showing the results for ﹩\mathrm{log}\left(\xi \right)﹩, we show the 2σ upper limit on ﹩\mathrm{log}\left(\xi \right)﹩ with the black solid lines.
Paper: The JCMT BISTRO-2 Survey: Magnetic Fields of the Massive DR21 Filament
Authors: Tao-Chung Ching, Keping Qiu, Di Li, Zhiyuan Ren, Shih-Ping Lai, David Berry, Kate Pattle, Ray Furuya, Derek Ward-Thompson, Doug Johnstone, Patrick M. Koch, Chang Won Lee, Thiem Hoang, Tetsuo Hasegawa, Woojin Kwon, Pierre Bastien, Chakali Eswaraiah, Jia-Wei Wang, Kyoung Hee Kim, Jihye Hwang, Archana Soam, A-Ran Lyo, Junhao Liu, Valentin J. M. Le Gouellec, Doris Arzoumanian, Anthony Whitworth, James Di Francesco, Frédérick Poidevin, Tie Liu, Simon Coudé, Mehrnoosh Tahani, Hong-Li Liu, Takashi Onaka, Dalei Li, Motohide Tamura, Zhiwei Chen, Xindi Tang, Florian Kirchschlager, Tyler L. Bourke, Do-Young Byun, Mike Chen, Huei-Ru Vivien Chen, Wen Ping Chen, Jungyeon Cho, Yunhee Choi, Youngwoo Choi, Minho Choi, Antonio Chrysostomou, Eun Jung Chung, Y. Sophia Dai, Pham Ngoc Diep, Yasuo Doi, Yan Duan, Hao-Yuan Duan, David Eden, Lapo Fanciullo, Jason Fiege, Laura M. Fissel, Erica Franzmann, Per Friberg, Rachel Friesen, Gary Fuller, Tim Gledhill, Sarah Graves, Jane Greaves, Matt Griffin, Qilao Gu, Ilseung Han, Saeko Hayashi, Martin Houde, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Il-Gyo Jeong, Vera Könyves, Ji-hyun Kang, Miju Kang, Janik Karoly, Akimasa Kataoka, Koji Kawabata, Francisca Kemper, Jongsoo Kim, Mi-Ryang Kim, Shinyoung Kim, Hyosung Kim, Kee-Tae Kim, Gwanjeong Kim, Jason Kirk, Masato I. N. Kobayashi, Takayoshi Kusune, Jungmi Kwon, Kevin Lacaille, Chi-Yan Law, Sang-Sung Lee, Hyeseung Lee, Jeong-Eun Lee, Chin-Fei Lee, Yong-Hee Lee, Guangxing Li, Hua-bai Li, Sheng-Jun Lin, Sheng-Yuan Liu, Xing Lu, Steve Mairs, Masafumi Matsumura, Brenda Matthews, Gerald Moriarty-Schieven, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Nguyen Bich Ngoc, Nagayoshi Ohashi, Geumsook Park, Harriet Parsons, Nicolas Peretto, Felix Priestley, Tae-Soo Pyo, Lei Qian, Ramprasad Rao, Mark Rawlings, Jonathan Rawlings, Brendan Retter, John Richer, Andrew Rigby, Sarah Sadavoy, Hiro Saito, Giorgio Savini, Masumichi Seta, Yoshito Shimajiri, Hiroko Shinnaga, Ya-Wen Tang, Kohji Tomisaka, Le Ngoc Tram, Yusuke Tsukamoto, Serena Viti, Hongchi Wang, Jintai Wu, Jinjin Xie, Meng-Zhe Yang, Hsi-Wei Yen, Hyunju Yoo, Jinghua Yuan, Hyeong-Sik Yun, Tetsuya Zenko, Chuan-Peng Zhang, Yapeng Zhang, Guoyin Zhang, Jianjun Zhou, Lei Zhu, Ilse de Looze, Philippe André, C. Darren Dowell, Stewart Eyres, Sam Falle, Jean-François Robitaille, Sven van Loo
Figure caption: The POL-2 dust polarization map at 850 μm toward the DR21 filament. The color scale represents the Stokes I intensity. The magnetic field segments plotted at intervals of 8″ show the magnetic field orientations, with lengths proportional to the polarization percentages. The JCMT 14.″1 beam is plotted at the bottom left corner. The positions of the 24 massive dense cores in Motte et al. (2007) are marked with filled black triangles and labeled in yellow, and the filamentary structures selected using filfinder are marked with orange dots along their crests. The names of the subfilaments following Hennemann et al. (2012) are labeled in yellow. The magnetic field segments of the subfilaments are shown in red color.
Paper: Conditions for Proton Temperature Anisotropy to Drive Instabilities in the Solar Wind
Authors: Simon Opie, Daniel Verscharen, Christopher H. K. Chen, Christopher J. Owen, Philip A. Isenberg
Figure caption: Panels (a)–(c) show the T ⊥ (red) and T ∥ (cyan) dependence on θ  BV  in the solar wind for (a) mirror-mode unstable (b) oblique firehose unstable and (c) all data. Panel (d) shows the equivalent dependency of T  R  (blue) and T  TN  (green) for all data. The results shown are running means over θ  BV  after sorting the data points by θ  BV .
Paper: Conditions for Proton Temperature Anisotropy to Drive Instabilities in the Solar Wind
Authors: Simon Opie, Daniel Verscharen, Christopher H. K. Chen, Christopher J. Owen, Philip A. Isenberg
Figure caption: PDF plots of persistence intervals in length scale for oblique firehose (green) and mirror-mode (magenta) instabilities in the solar wind. Panels (a) and (b) show the length scale in proton gyroradii (Δ ρ ). Panels (c) and (d) show the length scale in proton inertial lengths (Δ d ). We indicate break points at ﹩{{\rm{\Delta }}}_{b}^{\rho }﹩ with cyan vertical lines and power-law fits in dark blue, giving power indexes of ≈–2.17 for both the oblique firehose and the mirror-mode instability.