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arXiv 2023年

作者： Chase, Owen McBride, Felicia Gokus, Andrea Lucchini, Matteo Zhang, Haocheng Ojha, Roopesh Fox, Derek B. Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 United States Department of Physics and Astronomy Bowdoin College BrunswickME04011 United States Department of Physics Washington University in St. Louis One Brookings Drive St. LouisMO63130 United States McDonnell Center for the Space Sciences Washington University in St. Louis One Brookings Drive St. LouisMO63130 United States Dr. Karl Remeis-observatory & ECAP Friedrich-Alexander Universität Erlangen-Nürnberg Sternwartstr. 7 Bamberg96049 Germany Lehrstuhl für Astronomie Universität Würzburg Emil-Fischer-Strasse 31 Würzburg97074 Germany MIT Kavli Institute for Astrophysics and Space Research CambridgeMA02139 United States NASA Postdoctoral Program Fellow United States NASA Goddard Space Flight Center GreenbeltMD20771 United States NASA HQ 300 E St SW WashingtonDC20546-0002 United States

PKS 2005−489 is a well-known, bright southern BL Lac object that has been detected up to TeV energies. In a low-flux state it exhibits the expected multiwavelength double-peaked spectrum in the radio – γ-ray band. The high-flux state shows extreme flux variations in the X-ray band with a hardening as well as a peculiar curved feature in the spectrum. Thus far, PKS 2005−489 is the only source to exhibit such a feature. To study the X-ray variability further, we obtained the first hard X-ray spectrum of the source with NuSTAR. We compare quasi-simultaneous radio, optical, UV, soft and hard X-ray, and γ-ray data of PKS 2005−489 to archival data in order to study its broadband behavior. We find a very consistent quiet state in the SED, with little variation in spectral shape or flux between the 2012 and 2020 data. A possible explanation for the peculiar X-ray spectrum in the flaring state is an additional component in the jet, possibly accelerated via magnetic reconnection, that is not co-spatial to the low-flux state emission region. © 2023, CC BY.

关键词： Gamma rays

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Modeling Atmospheric Lines By the Exoplanet Community (MALBEC) version 1.0: A CUISINES radiative transfer intercomparison project

arXiv

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arXiv 2024年

作者： Villanueva, Geronimo L. Fauchez, Thomas J. Kofman, Vincent Alei, Eleonora Lee, Elspeth K.H. Janin, Estelle Himes, Michael D. Leconte, Jérémy Leung, Michaela Faggi, Sara Mak, Mei Ting Sergeev, Denis E. Kozakis, Thea Manners, James Mayne, Nathan Schwieterman, Edward W. Howe, Alex R. Batalha, Natasha NASA Goddard Space Flight Center GreenbeltMD United States Integrated Space Science and Technology Institute Department of Physics American University WashingtonDC United States NASA GSFC Sellers Exoplanet Environments Collaboration United States ETH Zurich Institute for Particle Physics & Astrophysics Wolfgang-Pauli-Str. 27 Zurich8093 Switzerland National Center of Competence in Research Planets Center for Space and Habitability University of Bern Gesellschaftsstrasse 6 BernCH-3012 Switzerland School of Earth and Space Exploration Arizona State University TempeAZ85281 United States Planetary Sciences Group Department of Physics University of Central Florida United States NASA Postdoctoral Program Fellow NASA Goddard Space Flight Center GreenbeltMD United States Laboratoire d’astrophysique de Bordeaux Univ. Bordeaux CNRS B18N allée Geoffroy Saint-Hilaire Pessac33615 France Department of Earth and Planetary Sciences University of California RiversideCA92521 United States Physics and Astronomy University of Exeter ExeterEX4 4QL United Kingdom National Space Institute Technical University of Denmark Elektrovej 328 Kgs. Lyngby2800 Denmark Met Office FitzRoy Road ExeterEX1 3PB United Kingdom Department of Earth and Planetary Sciences University of California RiversideCA United States NASA Goddard Space Flight Center 8800 Greenbelt Rd GreenbeltMD20771 United States Center for Research and Exploration in Space Science and Technology NASA/GSFC GreenbeltMD20771 United States NASA Ames Research Center Mountain ViewCA94035 United States

Radiative transfer (RT) models are critical in the interpretation of exoplanetary spectra, in simulating exoplanet climates and when designing the specifications of future flagship observatories. However, most models differ in methodologies and input data, which can lead to significantly different spectra. In this paper, we present the experimental protocol of the MALBEC (Modeling Atmospheric Lines By the Exoplanet Community) project. MALBEC is an exoplanet model intercomparison project (exoMIP) that belongs to the CUISINES (Climates Using Interactive Suites of Intercomparisons Nested for Exoplanet Studies) framework which aims to provide the exoplanet community with a large and diverse set of comparison and validation of models. The proposed protocol tests include a large set of initial participating RT models, a broad range of atmospheres (from Hot Jupiters to temperate terrestrials) and several observation geometries, which would allow us to quantify and compare the differences between different RT models used by the exoplanetary community. Two types of tests are proposed: transit spectroscopy and direct imaging modeling, with results from the proposed tests to be published in dedicated follow-up papers. To encourage the community to join this comparison effort and as an example, we present simulation results for one specific transit case (GJ-1214 b), in which we find notable differences in how the various codes handle the discretization of the atmospheres (e.g., sub-layering), the treatment of molecular opacities (e.g., correlated-k, line-by-line) and the default spectroscopic repositories generally used by each model (e.g., HITRAN, HITEMP, ExoMol). © 2024, CC BY.

关键词： Radiative transfer

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UV/Optical disk reverberation lags despite a faint X-ray corona in the AGN Mrk 335

arXiv

引用

arXiv 2023年

作者： Kara, Erin Barth, Aaron J. Cackett, Edward M. Gelbord, Jonathan Montano, John Li, Yan-Rong Santana, Lisabeth Horne, Keith Alston, William N. Buisson, Douglas Chelouche, Doron Du, Pu Fabian, Andrew C. Fian, Carina Gallo, Luigi Goad, Michael R. Grupe, Dirk González Buitrago, Diego H. Hernández Santisteban, Juan V. Kaspi, Shai Hu, Chen Komossa, S. Kriss, Gerard A. Lewin, Collin Lewis, Tiffany Loewenstein, Michael Lohfink, Anne Masterson, Megan McHardy, Ian M. Mehdipour, Missagh Miller, Jake Panagiotou, Christos Parker, Michael L. Pinto, Ciro Remillard, Ron Reynolds, Christopher Rogantini, Daniele Wang, Jian-Min Wang, Jingyi Wilkins, Dan MIT Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States Department of Physics and Astronomy 4129 Frederick Reines Hall University of California IrvineCA92697-4575 United States Department of Physics and Astronomy Wayne State University 666 W. Hancock St DetroitMI48201 United States Spectral Sciences Inc. 4 Fourth Ave. BurlingtonMA01803 United States Key Laboratory for Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences 19B Yuquan Road Beijing100049 China Department of Physics and Astronomy University of Pittsburgh 3941 O’Hara St PittsburghPA15260 United States SUPA School of Physics and Astronomy North Haugh St. AndrewsKY16 9SS United Kingdom Villanueva de la Canada MadridE-28691 Spain Department of Physics Faculty of Natural Sciences University of Haifa Haifa3498838 Israel Haifa Research Center for Theoretical Physics and Astrophysics University of Haifa Haifa3498838 Israel Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom School of Physics and Astronomy and Wise observatory Tel Aviv University Tel Aviv6997801 Israel Department of Astronomy and Physics Saint Mary’s University 923 Robie Street HalifaxNSB3H 3C3 Canada School of Physics and Astronomy University of Leicester University Road LeicesterLE1 7RH United Kingdom Department of Physics Geology and Engineering Technology Northern Kentucky University 1 Nunn Dr. Highland HeightsKY41099 United States Instituto de Astronomía Universidad Nacional Autónoma de México Km 103 Carretera Tijuana-Ensenada B.C. Ensenada22860 Mexico Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 Bonn53121 Germany Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States NASA Postdoctoral Program Fellow Astroparticle Physics Lab Goddard Space Flight Center United States Astrophysics Science Division NASA Goddard S

We present the first results from a 100-day Swift, NICER and ground-based X-ray/UV/optical reverberation mapping campaign of the Narrow-Line Seyfert 1 Mrk 335, when it was in an unprecedented low X-ray flux state. Despite dramatic suppression of the X-ray variability, we still observe UV/optical lags as expected from disk reverberation. Moreover, the UV/optical lags are consistent with archival observations when the X-ray luminosity was > 10 times higher. Interestingly, both low- and high-flux states reveal UV/optical lags that are 6 − 11 times longer than expected from a thin disk. These long lags are often interpreted as due to contamination from the broad line region, however the u band excess lag (containing the Balmer jump from the diffuse continuum) is less prevalent than in other AGN. The Swift campaign showed a low X-ray-to-optical correlation (similar to previous campaigns), but NICER and ground-based monitoring continued for another two weeks, during which the optical rose to the highest level of the campaign, followed ∼ 10 days later by a sharp rise in X-rays. While the low X-ray countrate and relatively large systematic uncertainties in the NICER background make this measurement challenging, if the optical does lead X-rays in this flare, this indicates a departure from the zeroth-order reprocessing picture. If the optical flare is due to an increase in mass accretion rate, this occurs on much shorter than the viscous timescale. Alternatively, the optical could be responding to an intrinsic rise in X-rays that is initially hidden from our line-of-sight. © 2023, CC BY.

关键词： Reverberation

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NuSTAR Observes Two Bulgeless Galaxies: No Hard X-ray AGN Detected in NGC 4178 or J0851+3926

arXiv

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arXiv 2022年

作者： Pfeifle, Ryan W. Satyapal, Shobita Ricci, Claudio Secrest, Nathan J. Gliozzi, Mario Bohn, Thomas Canalizo, Gabriela Reefe, Michael A. X-ray Astrophysics Laboratory NASA Goddard Space Flight Center Code 662 GreenbeltMD20771 United States Oak Ridge Associated Universities NASA NPP Program Oak RidgeTN37831 United States Department of Physics and Astronomy George Mason University 4400 University Drive MSN 3F3 FairfaxVA22030 United States Núcleo de Astronomía de la Facultad de Ingeniería Universidad Diego Portales Av. Ejército Libertador 441 Santiago Chile Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China U.S. Naval Observatory 3450 Massachusetts Avenue NW WashingtonDC20392 United States Hiroshima Astrophysical Science Center Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan University of California Riverside Department of Physics & Astronomy 900 University Ave. RiversideCA92521 United States Department of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA02139 United States NASA Postdoctoral Program National Science Foundation Graduate Research

The discovery over the last several decades of moderate luminosity AGNs in disk-dominated galaxies – which show no "classical" bulges – suggests that secular mechanisms represent an important growth pathway for supermassive black holes in these systems. We present new follow-up NuSTAR observations of the optically-elusive AGNs in two bulgeless galaxies, NGC 4178 and J0851+3926. NGC 4178 was originally reported as hosting an AGN based on the detection of [Ne V] mid-infrared emission detected by Spitzer, and based on Chandra X-ray imaging it has since been argued to host either a heavily obscured AGN or a supernova remnant. J0851+3926 was originally identified as an AGN based on its WISE mid-IR colors, and follow-up near-infrared spectroscopy previously revealed a hidden broad line region, offering compelling evidence for an optically-elusive AGN. Neither AGN is detected within the new NuSTAR imaging, and we derive upper limits on the hard X-ray 10-24 keV fluxes of −14 erg cm−2 s−1 and −14 erg cm−2 s−1 for the AGNs in NGC 4178 and J0851+3926, respectively. If these non-detections are due to large absorbing columns along the line of sight, the non-detections in NGC 4178 and J0851+3926 could be explained with column densities of log(NH/cm2) > 24.2 and log(NH/cm2) > 24.1, respectively. The nature of the nuclear activity in NGC 4178 remains inconclusive;it is plausible that the [Ne V] traces a period of higher activity in the past, but that the AGN is relatively quiescent now. The non-detection in J0851+3926 and multiwavelength properties are consistent with the AGN being heavily obscured. © 2022, CC BY.

关键词： Luminance

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Catalog of X-Ray Detected Be Stars (XDBS)

引用

Research Notes of the AAS 2022年第8期6卷 163-163页

作者： Caden Gobat Hui Yang Oleg Kargaltsev Jeremy Hare Igor Volkov Department of Physics The George Washington University 725 21st St NW Washington DC 20052 USA Southwest Research Institute 1050 Walnut Street Suite 300 Boulder CO 80302 USA NASA Goddard Space Flight Center Greenbelt MD 20771 USA NASA Postdoctoral Program Fellow

We present a catalog of X-ray Detected Be Stars (XDBS) with 161 Be stars from the Be Star Spectra (BeSS) database having X-ray counterparts in the Chandra Source Catalog v2.0, XMM-Newton 4XMM-DR11 Catalog, or Swift 2SXPS Catalog. The multi-wavelength catalog includes accurate optical positions, X-ray properties (fluxes, photon indices and hardness ratios), optical, near-infrared and infrared photometry, source classifications (when available), and other properties including proper motions, effective temperatures, X-ray to optical flux ratios as well. We also provide a convenient https://***/~kargaltsev/XDBS/graphical user interface which allows for easy visualization of the catalog content.

关键词： Catalogs Be stars X-ray stars X-ray binary stars

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Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE) II: Using Grid-Based Nested Sampling in Coronagraphy Observation Simulations for O2 and O3

arXiv

引用

arXiv 2023年

作者： Latouf, Natasha Mandell, Avi M. Villanueva, Geronimo L. Himes, Michael D. Moore, Michael Dane Susemiehl, Nicholas Crouse, Jaime Domagal-Goldman, Shawn Arney, Giada Kofman, Vincent Young, Amber V. Department of Physics and Astronomy George Mason University 4400 University Drive MS 3F3 FairfaxVA22030 United States NASA Goddard Space Flight Center 8800 Greenbelt Road GreenbeltMD20771 United States Sellers Exoplanents Environment Collaboration 8800 Greenbelt Road GreenbeltMD20771 United States NASA Postdoctoral Program Fellow NASA Goddard Space Flight Center 8800 Greenbelt Road GreenbeltMD20771 United States NASA Goddard Space Flight Center GreenbeltMD United States Business Integra Inc. BethesdaMD United States Sellers Exoplanets Environment Collaboration 8800 Greenbelt Road GreenbeltMD20771 United States Center for Research and Exploration in Space Science and Technology NASA Goddard Space Flight Center GreenbeltMD United States NASA Goddard Space Flight Center GreenbeltMD20771 United States NASA GSFC Sellers Exoplanet Environments Collaboration United States Integrated Space Science and Technology Institute Department of Physics American University WashingtonDC United States

We present the results for the detectability of the O2 and O3 molecular species in the atmosphere of an Earth-like planet using reflected light at visible wavelengths. By quantifying the detectability as a function of signal-to-noise ratio (SNR), we can constrain the best methods to detect these biosignatures with next-generation telescopes designed for high-contrast coronagraphy. Using 25 bandpasses between 0.515 and 1 µm) and a pre-constructed grid of geometric albedo spectra, we examined the spectral sensitivity needed to detect these species for a range of molecular abundances. We first replicate a modern-Earth twin atmosphere to study the detectability of current O2 and O3 levels, and then expand to a wider range of literature-driven abundances for each molecule. We constrain the optimal 20%, 30%, and 40% bandpasses based on the effective SNR of the data, and define the requirements for the possibility of simultaneous molecular detection. We present our findings of O2 and O3 detectability as functions of SNR, wavelength, and abundance, and discuss how to use these results for optimizing future instrument designs. We find that O2 is detectable between 0.64 and 0.83 µm with moderate-SNR data for abundances near that of modern-Earth and greater, but undetectable for lower abundances consistent with a Proterozoic Earth. O3 is detectable only at very high SNR data in the case of modern-Earth abundances, however it is detectable at low-SNR data for higher O3 abundances that can occur from efficient abiotic O3 production mechanisms. © 2023, CC0.

关键词： Signal to noise ratio

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Exploring the Correlation between Ha-to-UV Ratio and Burstiness for Typical Star-forming Galaxies at z ∼ 2

arXiv

引用

arXiv 2022年

作者： Rezaee, Saeed Reddy, Naveen A. Topping, Michael W. Shivaei, Irene Shapley, Alice E. Fetherolf, Tara Kriek, Mariska Coil, Alison Mobasher, Bahram Siana, Brian Du, Xinnan Khostovan, Ali Ahmad Weldon, Andrew Emami, Najmeh Chartab, Nima Department of Physics and Astronomy University of California RiversideCA92521 United States Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721 United States Nasa Hubble fellow United States Department of Physics and Astronomy University of California Los AngelesCA90095 United States Astronomy Department University of California BerkeleyCA94720 United States Center for Astrophysics and Space Sciences Department of Physics University of California San Diego 9500 Gilman Drive La Jolla CA92093 United States Kavli Institute for Particle Astrophysics & Cosmology Stanford University P. O. Box 2450 StanfordCA94305 United States Astrophysics Division NASA Goddard Space Flight Center GreenbeltMD20771 United States NASA Postdoctoral Program Fellow United States Minnesota Institute for Astrophysics University of Minnesota 116 Church St SE MinneapolisMN55455 United States The Observatories of the Carnegie Institution for Science 813 Santa Barbara St. PasadenaCA91101 United States

The Ha-to-UV luminosity ratio (L(Ha)/L(UV)) is often used to probe bursty star-formation histories (SFHs) of star-forming galaxies and it is important to validate it against other proxies for burstiness. To address this issue, we present a statistical analysis of the resolved distribution of star-formation-rate surface density (ΣSFR) as well as stellar age and their correlations with the globally measured L(Ha)/L(UV) for a sample of 310 star-forming galaxies in two redshift bins of 1.37 © 2022, CC BY.

关键词： Galaxies

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The long-stable hard state of XTE J1752−223 and the disk truncation dilemma

arXiv

引用

arXiv 2022年

作者： Connors, Riley M.T. García, Javier A. Tomsick, John Mastroserio, Guglielmo Grinberg, Victoria Steiner, James F. Jiang, Jiachen Fabian, Andrew C. Parker, Michael L. Harrison, Fiona Hare, Jeremy Mallick, Labani Lazar, Hadar Cahill Center for Astronomy and Astrophysics California Institute of Technology PasadenaCA91125 United States Dr Karl Remeis-Observatory Erlangen Centre for Astroparticle Physics Sternwartstr. 7 BambergD-96049 Germany Space Sciences Laboratory University of California Berkeley 7 Gauss Way BerkeleyCA94720-7450 United States Keplerlaan 1 Noordwk2201 AZ Netherlands MIT Kavli Institute 77 Massachusetts Avenue 37-241 CambridgeMA02139 United States Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom NASA Postdoctoral Program Fellow NASA Goddard Space Flight Center GreenbeltMD20771 United States

The degree to which the thin accretion disks of black hole X-ray binaries are truncated during hard spectral states remains a contentious open question in black hole astrophysics. During its singular observed outburst in 2009–2010, the black hole X-ray binary XTE J1752−223 spent ∼ 1 month in a long-stable hard spectral state at a luminosity of ∼ 0.02–0.1 LEdd. It was observed with 56 RXTE pointings during this period, with simultaneous Swift-XRT daily coverage during the first 10 days of the RXTE observations. Whilst reflection modeling has been extensively explored in the analysis of these data, there is a disagreement surrounding the geometry of the accretion disk and corona implied by the reflection features. We re-examine the combined, high signal-to-noise, simultaneous Swift and RXTE observations, and perform extensive reflection modeling with the latest relxill suite of reflection models, including newer high disk density models. We show that reflection modeling requires that the disk be within ∼ 5 RISCO during the hard spectral state, whilst weaker constraints from the thermal disk emission imply higher truncation (Rin = 6–80 RISCO). We also explore more complex coronal continuum models, allowing for two Comptonization components instead of one, and show that the reflection features still require only a mildly truncated disk. Finally we present a full comparison of our results to previous constraints found from analyses of the same dataset. © 2022, CC BY-NC-ND.

关键词： Black holes

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Determining the nanoflare heating frequency of an X-ray Bright Point observed by MaGIXS

arXiv

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arXiv 2024年

作者： Mondal, Biswajit Athiray, P.S. Winebarger, Amy R. Savage, Sabrina L. Kobayashi, Ken Bradshaw, Stephen Barnes, Will Champey, Patrick R. Cheimets, Peter Dudík, Jaroslav Golub, Leon Mason, Helen E. McKenzie, David E. Moore, Christopher S. Madsen, Chad Reeves, Katharine K. Testa, Paola Vigil, Genevieve D. Warren, Harry P. Walsh, Robert W. Del Zanna, Giulio NASA Postdoctoral Program NASA Marshall Space Flight Center ST13 HuntsvilleAL United States Center for Space Plasma and Aeronomic Research The University of Alabama in Huntsville HuntsvilleAL United States NASA Marshall Space Flight Center ST13 HuntsvilleAL United States Rice University 6100 Main Street HoustonTX77005 United States Department of Physics American University WashingtonDC United States NASA Goddard Space Flight Center Heliophysics Science Division GreenbeltMD20771 United States Center for Astrophysics — Harvard & Smithsonian CambridgeMA02138 United States Astronomical Institute Czech Academy of Sciences Fricova 298 Ondrejov25165 Czech Republic DAMTP Centre for Mathematical Sciences University of Cambridge Wilberforce Road CambridgeCB3 0WA United Kingdom Space Science Division Naval Research Laboratory WashingtonDC20375 United States University of Central Lancashire PrestonPR1 2HE United Kingdom

Nanoflares are thought to be one of the prime candidates that can heat the solar corona to its multi-million kelvin temperature. Individual nanoflares are difficult to detect with the present generation instruments, however their presence can be inferred by comparing simulated nanoflare-heated plasma emissions with the observed emission. Using HYDRAD coronal loop simulations, we model the emission from an X-ray bright point (XBP) observed by the Marshall Grazing Incidence X-ray Spectrometer (MaGIXS), along with nearest-available observations from the Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) and X-Ray Telescope (XRT) onboard Hinode observatory. The length and magnetic field strength of the coronal loops are derived from the linear-force-free extrapolation of the observed photospheric magnetogram by Helioseismic and Magnetic Imager (HMI) onboard SDO. Each loop is assumed to be heated by random nanoflares, whose magnitude and frequency are determined by the loop length and magnetic field strength. The simulation results are then compared and matched against the measured intensity from AIA, XRT, and MaGIXS. Our model results indicate the observed emissions from the XBP under study could be well matched by a distribution of nanoflares with average delay times 1500 s to 3000 s, which suggest that the heating is dominated by high-frequency events. Further, we demonstrate the high sensitivity of MaGIXS and XRT to diagnose the heating frequency using this method, while AIA passbands are found to be the least sensitive. © 2024, CC BY-NC-ND.

关键词： Observatories

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On the Mesoscale Structure of CMEs at Mercury's Orbit: BepiColombo and Parker Solar Probe Observations

arXiv

引用

arXiv 2024年

作者： Palmerio, Erika Carcaboso, Fernando Khoo, Leng Ying Salman, Tarik M. Sánchez-Cano, Beatriz Lynch, Benjamin J. Rivera, Yeimy J. Pal, Sanchita Nieves-Chinchilla, Teresa Weiss, Andreas J. Lario, David Mieth, Johannes Z.D. Heyner, Daniel Stevens, Michael L. Romeo, Orlando M. Zhukov, Andrei N. Rodriguez, Luciano Lee, Christina O. Cohen, Christina M.S. Rodríguez-García, Laura Whittlesey, Phyllis L. Dresing, Nina Oleynik, Philipp Jebaraj, Immanuel C. Fischer, David Schmid, Daniel Richter, Ingo Auster, Hans-Ulrich Fraschetti, Federico Mierla, Marilena Predictive Science Inc. San DiegoCA92121 United States Postdoctoral Program Fellow NASA Goddard Space Flight Center GreenbeltMD20771 United States Department of Astrophysical Sciences Princeton University PrincetonNJ08544 United States Heliophysics Science Division NASA Goddard Space Flight Center GreenbeltMD20771 United States Department of Physics and Astronomy George Mason University FairfaxVA22030 United States School of Physics and Astronomy University of Leicester LeicesterLE1 7RH United Kingdom Space Sciences Laboratory University of California BerkeleyCA94720 United States Department of Earth Planetary and Space Sciences University of California Los AngelesCA90095 United States Center for Astrophysics Harvard & Smithsonian CambridgeMA02138 United States Institut für Geophysik und extraterrestrische Physik TU Braunschweig BraunschweigD-38106 Germany Department of Earth and Planetary Science University of California BerkeleyCA94720 United States Solar–Terrestrial Centre of Excellence—SIDC Royal Observatory of Belgium BrusselsB-1180 Belgium Skobeltsyn Institute of Nuclear Physics Moscow State University Moscow119991 Russia California Institute of Technology PasadenaCA91125 United States European Space Astronomy Centre European Space Agency Villanueva de la Cañada MadridE-28692 Spain Alcalá de Henares MadridE-28801 Spain Department of Physics and Astronomy University of Turku TurkuFI-20014 Finland Space Research Institute Austrian Academy of Sciences GrazA-8042 Austria Department of Planetary Sciences Lunar and Planetary Lab TucsonAZ85721 United States Institute of Geodynamics The Romanian Academy Bucharest020032 37 Romania

On 2022 February 15, an impressive filament eruption was observed off the solar eastern limb from three remote-sensing viewpoints, namely Earth, STEREO-A, and Solar Orbiter. In addition to representing the most-distant observed filament at extreme ultraviolet wavelengths—captured by Solar Orbiter’s field of view extending to above 6 R☉—this event was also associated with the release of a fast (∼2200 km·s−1) coronal mass ejection (CME) that was directed towards BepiColombo and Parker Solar Probe. These two probes were separated by 2◦ in latitude, 4◦ in longitude, and 0.03 au in radial distance around the time of the CME-driven shock arrival in situ. The relative proximity of the two probes to each other and to the Sun (∼0.35 au) allows us to study the mesoscale structure of CMEs at Mercury’s orbit for the first time. We analyse similarities and differences in the main CME-related structures measured at the two locations, namely the interplanetary shock, the sheath region, and the magnetic ejecta. We find that, despite the separation between the two spacecraft being well within the typical uncertainties associated with determination of CME geometric parameters from remote-sensing observations, the two sets of in-situ measurements display some profound differences that make understanding of the overall 3D CME structure particularly challenging. Finally, we discuss our findings within the context of space weather at Mercury’s distances and in terms of the need to investigate solar transients via spacecraft constellations with small separations, which has been gaining significant attention during recent years. © 2024, CC BY.

关键词： Probes

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