Pub Date : 2023-11-03DOI: 10.1007/s11214-023-01018-1
Ilya Usoskin, Fusa Miyake, Melanie Baroni, Nicolas Brehm, Silvia Dalla, Hisashi Hayakawa, Hugh Hudson, A. J. Timothy Jull, Delores Knipp, Sergey Koldobskiy, Hiroyuki Maehara, Florian Mekhaldi, Yuta Notsu, Stepan Poluianov, Eugene Rozanov, Alexander Shapiro, Tobias Spiegl, Timofei Sukhodolov, Joonas Uusitalo, Lukas Wacker
Abstract The Sun is magnetically active and often produces eruptive events on different energetic and temporal scales. Until recently, the upper limit of such events was unknown and believed to be roughly represented by direct instrumental observations. However, two types of extreme events were discovered recently: extreme solar energetic particle events on the multi-millennial time scale and super-flares on sun-like stars. Both discoveries imply that the Sun might rarely produce events, called extreme solar events (ESE), whose energy could be orders of magnitude greater than anything we have observed during recent decades. During the years following these discoveries, great progress has been achieved in collecting observational evidence, uncovering new events, making statistical analyses, and developing theoretical modelling. The ESE paradigm lives and is being developed. On the other hand, many outstanding questions still remain open and new ones emerge. Here we present an overview of the current state of the art and the forming paradigm of ESE from different points of view: solar physics, stellar–solar projections, cosmogenic-isotope data, modelling, historical data, as well as terrestrial, technological and societal effects of ESEs. Special focus is paid to open questions and further developments. This review is based on the joint work of the International Space Science Institute (ISSI) team #510 (2020–2022).
{"title":"Extreme Solar Events: Setting up a Paradigm","authors":"Ilya Usoskin, Fusa Miyake, Melanie Baroni, Nicolas Brehm, Silvia Dalla, Hisashi Hayakawa, Hugh Hudson, A. J. Timothy Jull, Delores Knipp, Sergey Koldobskiy, Hiroyuki Maehara, Florian Mekhaldi, Yuta Notsu, Stepan Poluianov, Eugene Rozanov, Alexander Shapiro, Tobias Spiegl, Timofei Sukhodolov, Joonas Uusitalo, Lukas Wacker","doi":"10.1007/s11214-023-01018-1","DOIUrl":"https://doi.org/10.1007/s11214-023-01018-1","url":null,"abstract":"Abstract The Sun is magnetically active and often produces eruptive events on different energetic and temporal scales. Until recently, the upper limit of such events was unknown and believed to be roughly represented by direct instrumental observations. However, two types of extreme events were discovered recently: extreme solar energetic particle events on the multi-millennial time scale and super-flares on sun-like stars. Both discoveries imply that the Sun might rarely produce events, called extreme solar events (ESE), whose energy could be orders of magnitude greater than anything we have observed during recent decades. During the years following these discoveries, great progress has been achieved in collecting observational evidence, uncovering new events, making statistical analyses, and developing theoretical modelling. The ESE paradigm lives and is being developed. On the other hand, many outstanding questions still remain open and new ones emerge. Here we present an overview of the current state of the art and the forming paradigm of ESE from different points of view: solar physics, stellar–solar projections, cosmogenic-isotope data, modelling, historical data, as well as terrestrial, technological and societal effects of ESEs. Special focus is paid to open questions and further developments. This review is based on the joint work of the International Space Science Institute (ISSI) team #510 (2020–2022).","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-11-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135819336","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-31DOI: 10.1007/s11214-023-01022-5
Thomas Widemann, Suzanne E. Smrekar, James B. Garvin, Anne Grete Straume-Lindner, Adriana C. Ocampo, Mitchell D. Schulte, Thomas Voirin, Scott Hensley, M. Darby Dyar, Jennifer L. Whitten, Daniel C. Nunes, Stephanie A. Getty, Giada N. Arney, Natasha M. Johnson, Erika Kohler, Tilman Spohn, Joseph G. O’Rourke, Colin F. Wilson, Michael J. Way, Colby Ostberg, Frances Westall, Dennis Höning, Seth Jacobson, Arnaud Salvador, Guillaume Avice, Doris Breuer, Lynn Carter, Martha S. Gilmore, Richard Ghail, Jörn Helbert, Paul Byrne, Alison R. Santos, Robert R. Herrick, Noam Izenberg, Emmanuel Marcq, Tobias Rolf, Matt Weller, Cedric Gillmann, Oleg Korablev, Lev Zelenyi, Ludmila Zasova, Dmitry Gorinov, Gaurav Seth, C. V. Narasimha Rao, Nilesh Desai
{"title":"Correction to: Venus Evolution Through Time: Key Science Questions, Selected Mission Concepts and Future Investigations","authors":"Thomas Widemann, Suzanne E. Smrekar, James B. Garvin, Anne Grete Straume-Lindner, Adriana C. Ocampo, Mitchell D. Schulte, Thomas Voirin, Scott Hensley, M. Darby Dyar, Jennifer L. Whitten, Daniel C. Nunes, Stephanie A. Getty, Giada N. Arney, Natasha M. Johnson, Erika Kohler, Tilman Spohn, Joseph G. O’Rourke, Colin F. Wilson, Michael J. Way, Colby Ostberg, Frances Westall, Dennis Höning, Seth Jacobson, Arnaud Salvador, Guillaume Avice, Doris Breuer, Lynn Carter, Martha S. Gilmore, Richard Ghail, Jörn Helbert, Paul Byrne, Alison R. Santos, Robert R. Herrick, Noam Izenberg, Emmanuel Marcq, Tobias Rolf, Matt Weller, Cedric Gillmann, Oleg Korablev, Lev Zelenyi, Ludmila Zasova, Dmitry Gorinov, Gaurav Seth, C. V. Narasimha Rao, Nilesh Desai","doi":"10.1007/s11214-023-01022-5","DOIUrl":"https://doi.org/10.1007/s11214-023-01022-5","url":null,"abstract":"","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-10-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135871358","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-30DOI: 10.1007/s11214-023-01010-9
K.-J. Hwang, R. Nakamura, J. P. Eastwood, S. A. Fuselier, H. Hasegawa, T. Nakamura, B. Lavraud, K. Dokgo, D. L. Turner, R. E. Ergun, P. H. Reiff
Abstract Various physical processes in association with magnetic reconnection occur over multiple scales from the microscopic to macroscopic scale lengths. This paper reviews multi-scale and cross-scale aspects of magnetic reconnection revealed in the near-Earth space beyond the general global-scale features and magnetospheric circulation organized by the Dungey Cycle. Significant and novel advancements recently reported, in particular, since the launch of the Magnetospheric Multi-scale mission (MMS), are highlighted being categorized into different locations with different magnetic topologies. These potentially paradigm-shifting findings include shock and foreshock transient driven reconnection, magnetosheath turbulent reconnection, flow shear driven reconnection, multiple X-line structures generated in the dayside/flankside/nightside magnetospheric current sheets, development and evolution of reconnection-driven structures such as flux transfer events, flux ropes, and dipolarization fronts, and their interactions with ambient plasmas. The paper emphasizes key aspects of kinetic processes leading to multi-scale structures and bringing large-scale impacts of magnetic reconnection as discovered in the geospace environment. These key features can be relevant and applicable to understanding other heliospheric and astrophysical systems.
{"title":"Cross-Scale Processes of Magnetic Reconnection","authors":"K.-J. Hwang, R. Nakamura, J. P. Eastwood, S. A. Fuselier, H. Hasegawa, T. Nakamura, B. Lavraud, K. Dokgo, D. L. Turner, R. E. Ergun, P. H. Reiff","doi":"10.1007/s11214-023-01010-9","DOIUrl":"https://doi.org/10.1007/s11214-023-01010-9","url":null,"abstract":"Abstract Various physical processes in association with magnetic reconnection occur over multiple scales from the microscopic to macroscopic scale lengths. This paper reviews multi-scale and cross-scale aspects of magnetic reconnection revealed in the near-Earth space beyond the general global-scale features and magnetospheric circulation organized by the Dungey Cycle. Significant and novel advancements recently reported, in particular, since the launch of the Magnetospheric Multi-scale mission (MMS), are highlighted being categorized into different locations with different magnetic topologies. These potentially paradigm-shifting findings include shock and foreshock transient driven reconnection, magnetosheath turbulent reconnection, flow shear driven reconnection, multiple X-line structures generated in the dayside/flankside/nightside magnetospheric current sheets, development and evolution of reconnection-driven structures such as flux transfer events, flux ropes, and dipolarization fronts, and their interactions with ambient plasmas. The paper emphasizes key aspects of kinetic processes leading to multi-scale structures and bringing large-scale impacts of magnetic reconnection as discovered in the geospace environment. These key features can be relevant and applicable to understanding other heliospheric and astrophysical systems.","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-10-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136067798","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-30DOI: 10.1007/s11214-023-01016-3
Emre Işık, Jennifer L. van Saders, Ansgar Reiners, Travis S. Metcalfe
Abstract Magnetic activity is a ubiquitous feature of stars with convective outer layers, with implications from stellar evolution to planetary atmospheres. Investigating the mechanisms responsible for the observed stellar activity signals from days to billions of years is important in deepening our understanding of the spatial configurations and temporal patterns of stellar dynamos, including that of the Sun. In this paper, we focus on three problems and their possible solutions. We start with direct field measurements and show how they probe the dependence of magnetic flux and its density on stellar properties and activity indicators. Next, we review the current state-of-the-art in physics-based models of photospheric activity patterns and their variation from rotational to activity-cycle timescales. We then outline the current state of understanding in the long-term evolution of stellar dynamos, first by using chromospheric and coronal activity diagnostics, then with model-based implications on magnetic braking, which is the key mechanism by which stars spin down and become inactive as they age. We conclude by discussing possible directions to improve the modeling and analysis of stellar magnetic fields.
{"title":"Scaling and Evolution of Stellar Magnetic Activity","authors":"Emre Işık, Jennifer L. van Saders, Ansgar Reiners, Travis S. Metcalfe","doi":"10.1007/s11214-023-01016-3","DOIUrl":"https://doi.org/10.1007/s11214-023-01016-3","url":null,"abstract":"Abstract Magnetic activity is a ubiquitous feature of stars with convective outer layers, with implications from stellar evolution to planetary atmospheres. Investigating the mechanisms responsible for the observed stellar activity signals from days to billions of years is important in deepening our understanding of the spatial configurations and temporal patterns of stellar dynamos, including that of the Sun. In this paper, we focus on three problems and their possible solutions. We start with direct field measurements and show how they probe the dependence of magnetic flux and its density on stellar properties and activity indicators. Next, we review the current state-of-the-art in physics-based models of photospheric activity patterns and their variation from rotational to activity-cycle timescales. We then outline the current state of understanding in the long-term evolution of stellar dynamos, first by using chromospheric and coronal activity diagnostics, then with model-based implications on magnetic braking, which is the key mechanism by which stars spin down and become inactive as they age. We conclude by discussing possible directions to improve the modeling and analysis of stellar magnetic fields.","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-10-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136103867","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-25DOI: 10.1007/s11214-023-01009-2
D. C. Reuter, A. A. Simon, A. Lunsford, H. Kaplan, M. Garrison, J. Simpson, G. Casto, Z. Dolch, P. Finneran, W. Grundy, C. Howett, P. Kim, M. Loose, T. Null, F. Parong, J. Rodriguez-ruiz, P. Roming, K. Smith, P. Thompson, B. Tokarcik, T. Veach, S. Wall, J. Ward, E. Weigle, H. Levison
Abstract The Lucy Mission to the Trojan asteroids in Jupiter’s orbit carries an instrument named L’Ralph, a visible/near infrared multi-spectral imager and a short wavelength infrared hyperspectral imager. It is one of the core instruments on Lucy, NASA’s first mission to the Trojans. L’Ralph’s primary purpose is to map the surface geology and composition of these objects, but it will also be used to search for possible tenuous exospheres. It is compact, low mass (32.3 kg), power efficient (24.5 W), and robust with high sensitivity and excellent imaging. These characteristics, and its high degree of redundancy, make L’Ralph ideally suited to this long-duration multi-flyby reconnaissance mission.
{"title":"L’Ralph: A Visible/Infrared Spectral Imager for the Lucy Mission to the Trojans","authors":"D. C. Reuter, A. A. Simon, A. Lunsford, H. Kaplan, M. Garrison, J. Simpson, G. Casto, Z. Dolch, P. Finneran, W. Grundy, C. Howett, P. Kim, M. Loose, T. Null, F. Parong, J. Rodriguez-ruiz, P. Roming, K. Smith, P. Thompson, B. Tokarcik, T. Veach, S. Wall, J. Ward, E. Weigle, H. Levison","doi":"10.1007/s11214-023-01009-2","DOIUrl":"https://doi.org/10.1007/s11214-023-01009-2","url":null,"abstract":"Abstract The Lucy Mission to the Trojan asteroids in Jupiter’s orbit carries an instrument named L’Ralph, a visible/near infrared multi-spectral imager and a short wavelength infrared hyperspectral imager. It is one of the core instruments on Lucy, NASA’s first mission to the Trojans. L’Ralph’s primary purpose is to map the surface geology and composition of these objects, but it will also be used to search for possible tenuous exospheres. It is compact, low mass (32.3 kg), power efficient (24.5 W), and robust with high sensitivity and excellent imaging. These characteristics, and its high degree of redundancy, make L’Ralph ideally suited to this long-duration multi-flyby reconnaissance mission.","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-10-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135216036","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-24DOI: 10.1007/s11214-023-01014-5
J. Henneke, D. Klevang, Y. Liu, J. Jørgensen, T. Denver, M. Rice, S. VanBommel, C. Toldbo, J. Hurowitz, M. Tice, N. Tosca, J. Johnson, A. Winhold, A. Allwood, J. Bell
Abstract The Planetary Instrument for X-ray Lithochemistry (PIXL) onboard the Perseverance rover, part of NASA’s Mars 2020 mission, has the first camera system that utilizes active light sources to generate multispectral data directly on a planetary surface. PIXL collects the multispectral data using three different components in the Optical Fiducial System (OFS): Micro Context Camera (MCC), Floodlight Illuminator (FLI), and Structure light illuminator (SLI). MCC captures images illuminated at different wavelengths by FLI while topography information is obtained by synchronously operating the MCC and SLI. A radiometric calibration for such a system has not been attempted before. Here we present a novel radiometric correction process and verify the output to a mean error of 0.4% by comparing it to calibrated spectral data from the Three Axis N-sample Automated Goniometer for Evaluation Reflectance (TANAGER). We demonstrate that the radiometrically corrected data can clearly discern different features in natural rock and mineral samples. We also conclude that the same radiometric correction process can be used on Mars as the optical system is designed to autonomously compensates for the effects of the Martian environment on the instrument. Having multispectral capabilities has proven to be very valuable for extrapolating the detailed mineral and crystallographic information produced by X-ray spectroscopy from the X-ray system of PIXL.
{"title":"A Radiometric Correction Method and Performance Characteristics for PIXL’s Multispectral Analysis Using LEDs","authors":"J. Henneke, D. Klevang, Y. Liu, J. Jørgensen, T. Denver, M. Rice, S. VanBommel, C. Toldbo, J. Hurowitz, M. Tice, N. Tosca, J. Johnson, A. Winhold, A. Allwood, J. Bell","doi":"10.1007/s11214-023-01014-5","DOIUrl":"https://doi.org/10.1007/s11214-023-01014-5","url":null,"abstract":"Abstract The Planetary Instrument for X-ray Lithochemistry (PIXL) onboard the Perseverance rover, part of NASA’s Mars 2020 mission, has the first camera system that utilizes active light sources to generate multispectral data directly on a planetary surface. PIXL collects the multispectral data using three different components in the Optical Fiducial System (OFS): Micro Context Camera (MCC), Floodlight Illuminator (FLI), and Structure light illuminator (SLI). MCC captures images illuminated at different wavelengths by FLI while topography information is obtained by synchronously operating the MCC and SLI. A radiometric calibration for such a system has not been attempted before. Here we present a novel radiometric correction process and verify the output to a mean error of 0.4% by comparing it to calibrated spectral data from the Three Axis N-sample Automated Goniometer for Evaluation Reflectance (TANAGER). We demonstrate that the radiometrically corrected data can clearly discern different features in natural rock and mineral samples. We also conclude that the same radiometric correction process can be used on Mars as the optical system is designed to autonomously compensates for the effects of the Martian environment on the instrument. Having multispectral capabilities has proven to be very valuable for extrapolating the detailed mineral and crystallographic information produced by X-ray spectroscopy from the X-ray system of PIXL.","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-10-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135267045","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-20DOI: 10.1007/s11214-023-01015-4
Marica Branchesi, Maurizio Falanga, Jan Harms, Karan Jani, Stavros Katsanevas, Philippe Lognonné, Francesca Badaracco, Luigi Cacciapuoti, Enrico Cappellaro, Simone Dell’Agnello, Sébastien de Raucourt, Alessandro Frigeri, Domenico Giardini, Oliver Jennrich, Taichi Kawamura, Valeriya Korol, Martin Landrø, Josipa Majstorović, Piyush Marmat, Paolo Mazzali, Marco Muccino, Ferdinando Patat, Elena Pian, Tsvi Piran, Severine Rosat, Sheila Rowan, Simon Stähler, Jacopo Tissino
Abstract A new era of lunar exploration has begun bringing immense opportunities for science as well. It has been proposed to deploy a new generation of observatories on the lunar surface for deep studies of our Universe. This includes radio antennas, which would be protected on the far side of the Moon from terrestrial radio interference, and gravitational-wave (GW) detectors, which would profit from the extremely low level of seismic disturbances on the Moon. In recent years, novel concepts have been proposed for lunar GW detectors based on long-baseline laser interferometry or on compact sensors measuring the lunar surface vibrations caused by GWs. In this article, we review the concepts and science opportunities for such instruments on the Moon. In addition to promising breakthrough discoveries in astrophysics and cosmology, lunar GW detectors would also be formidable probes of the lunar internal structure and improve our understanding of the lunar geophysical environment.
{"title":"Lunar Gravitational-Wave Detection","authors":"Marica Branchesi, Maurizio Falanga, Jan Harms, Karan Jani, Stavros Katsanevas, Philippe Lognonné, Francesca Badaracco, Luigi Cacciapuoti, Enrico Cappellaro, Simone Dell’Agnello, Sébastien de Raucourt, Alessandro Frigeri, Domenico Giardini, Oliver Jennrich, Taichi Kawamura, Valeriya Korol, Martin Landrø, Josipa Majstorović, Piyush Marmat, Paolo Mazzali, Marco Muccino, Ferdinando Patat, Elena Pian, Tsvi Piran, Severine Rosat, Sheila Rowan, Simon Stähler, Jacopo Tissino","doi":"10.1007/s11214-023-01015-4","DOIUrl":"https://doi.org/10.1007/s11214-023-01015-4","url":null,"abstract":"Abstract A new era of lunar exploration has begun bringing immense opportunities for science as well. It has been proposed to deploy a new generation of observatories on the lunar surface for deep studies of our Universe. This includes radio antennas, which would be protected on the far side of the Moon from terrestrial radio interference, and gravitational-wave (GW) detectors, which would profit from the extremely low level of seismic disturbances on the Moon. In recent years, novel concepts have been proposed for lunar GW detectors based on long-baseline laser interferometry or on compact sensors measuring the lunar surface vibrations caused by GWs. In this article, we review the concepts and science opportunities for such instruments on the Moon. In addition to promising breakthrough discoveries in astrophysics and cosmology, lunar GW detectors would also be formidable probes of the lunar internal structure and improve our understanding of the lunar geophysical environment.","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-10-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135616057","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-19DOI: 10.1007/s11214-023-01012-7
Marius Anger, Petri Niemelä, Kiril Cheremetiev, Bruce Clayhills, Anton Fetzer, Ville Lundén, Markus Hiltunen, Tomi Kärkkäinen, M. Mayank, Lucile Turc, Adnane Osmane, Minna Palmroth, Emilia Kilpua, Philipp Oleynik, Rami Vainio, Pasi Virtanen, Petri Toivanen, Pekka Janhunen, David Fischer, Guillaume Le Bonhomme, Andris Slavinskis, Jaan Praks
Abstract Earth’s radiation belts are extremely important for space weather because they can store and accelerate particles to relativistic energies, which can have a potential impact on satellite functionality, communications, and navigation systems. The FORESAIL consortium wants to measure these high-energy particle fluxes to understand the dynamics of the radiation belts with its satellite mission Foresail-2. The mission aims to measure magnetic ultra low frequency waves and the plasma environment in the magnetosphere around Earth. The captured data will help to improve our understanding of space weather, and in particular the dynamics of Earth’s radiation belts during periods of large disturbances inside the magnetosphere. A mission design analysis and several trade-off studies are conducted to find the requirements for the science payloads and spacecraft avionics design. Deducted from these requirements, four different payloads are proposed to gather science data in a highly elliptical orbit such as a geostationary transfer orbit. The precision magnetometer uses flux-gate technology to measure magnetic waves from 1 mHz to 10 Hz. The spin scanning particle telescope is built around a detector stack to measure electron spectra in the range of 30 keV to 10 MeV. Additionally, this mission serves as a technology demonstrator for the Coulomb drag experiment which proposes a new kind of electric solar wind sail utilising the Coulomb drag force imposed onto a 300 m long tether. The fourth payload investigates multilayer radiation shielding and single event effects. All payloads will be supported by a newly developed 6U platform using mostly commercial off-the-shelf components. Its proposed avionics face several unique design requirements rising from the payloads and the preferred highly elliptical orbit for this mission.
{"title":"Foresail-2: Space Physics Mission in a Challenging Environment","authors":"Marius Anger, Petri Niemelä, Kiril Cheremetiev, Bruce Clayhills, Anton Fetzer, Ville Lundén, Markus Hiltunen, Tomi Kärkkäinen, M. Mayank, Lucile Turc, Adnane Osmane, Minna Palmroth, Emilia Kilpua, Philipp Oleynik, Rami Vainio, Pasi Virtanen, Petri Toivanen, Pekka Janhunen, David Fischer, Guillaume Le Bonhomme, Andris Slavinskis, Jaan Praks","doi":"10.1007/s11214-023-01012-7","DOIUrl":"https://doi.org/10.1007/s11214-023-01012-7","url":null,"abstract":"Abstract Earth’s radiation belts are extremely important for space weather because they can store and accelerate particles to relativistic energies, which can have a potential impact on satellite functionality, communications, and navigation systems. The FORESAIL consortium wants to measure these high-energy particle fluxes to understand the dynamics of the radiation belts with its satellite mission Foresail-2. The mission aims to measure magnetic ultra low frequency waves and the plasma environment in the magnetosphere around Earth. The captured data will help to improve our understanding of space weather, and in particular the dynamics of Earth’s radiation belts during periods of large disturbances inside the magnetosphere. A mission design analysis and several trade-off studies are conducted to find the requirements for the science payloads and spacecraft avionics design. Deducted from these requirements, four different payloads are proposed to gather science data in a highly elliptical orbit such as a geostationary transfer orbit. The precision magnetometer uses flux-gate technology to measure magnetic waves from 1 mHz to 10 Hz. The spin scanning particle telescope is built around a detector stack to measure electron spectra in the range of 30 keV to 10 MeV. Additionally, this mission serves as a technology demonstrator for the Coulomb drag experiment which proposes a new kind of electric solar wind sail utilising the Coulomb drag force imposed onto a 300 m long tether. The fourth payload investigates multilayer radiation shielding and single event effects. All payloads will be supported by a newly developed 6U platform using mostly commercial off-the-shelf components. Its proposed avionics face several unique design requirements rising from the payloads and the preferred highly elliptical orbit for this mission.","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-10-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135666815","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-17DOI: 10.1007/s11214-023-01008-3
Aimee Norton, Rachel Howe, Lisa Upton, Ilya Usoskin
Abstract We describe the defining observations of the solar cycle that provide constraints for the dynamo processes operating within the Sun. Specifically, we report on the following topics: historical sunspot numbers and revisions; active region (AR) flux ranges and lifetimes; bipolar magnetic region tilt angles; Hale and Joy’s law; the impact of rogue ARs on cycle progression and the amplitude of the following cycle; the spatio-temporal emergence of ARs that creates the butterfly diagram; polar fields; large-scale flows including zonal, meridional, and AR in-flows; short-term cycle variability; and helioseismic results including mode parameter changes.
{"title":"Solar Cycle Observations","authors":"Aimee Norton, Rachel Howe, Lisa Upton, Ilya Usoskin","doi":"10.1007/s11214-023-01008-3","DOIUrl":"https://doi.org/10.1007/s11214-023-01008-3","url":null,"abstract":"Abstract We describe the defining observations of the solar cycle that provide constraints for the dynamo processes operating within the Sun. Specifically, we report on the following topics: historical sunspot numbers and revisions; active region (AR) flux ranges and lifetimes; bipolar magnetic region tilt angles; Hale and Joy’s law; the impact of rogue ARs on cycle progression and the amplitude of the following cycle; the spatio-temporal emergence of ARs that creates the butterfly diagram; polar fields; large-scale flows including zonal, meridional, and AR in-flows; short-term cycle variability; and helioseismic results including mode parameter changes.","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-10-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136032848","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-17DOI: 10.1007/s11214-023-01006-5
Maria A. Weber, Hannah Schunker, Laurène Jouve, Emre Işık
Abstract The emergence of active regions on the Sun is an integral feature of the solar dynamo mechanism. However, details about the generation of active-region-scale magnetism and the journey of this magnetic flux from the interior to the photosphere are still in question. Shifting paradigms are now developing for the source depth of the Sun’s large-scale magnetism, the organization of this magnetism into fibril flux tubes, and the role of convection in shaping active-region observables. Here we review the landscape of flux emergence theories and simulations, highlight the role flux emergence plays in the global dynamo process, and make connections between flux emergence on the Sun and other cool stars. As longer-term and higher fidelity observations of both solar active regions and their associated flows are amassed, it is now possible to place new constraints on models of emerging flux. We discuss the outcomes of statistical studies which provide observational evidence that flux emergence may be a more passive process (at least in the upper convection zone); dominated to a greater extent by the influence of convection and to a lesser extent by buoyancy and the Coriolis force acting on rising magnetic flux tubes than previously thought. We also discuss how the relationship between stellar rotation, fractional convection zone depth, and magnetic activity on other stars can help us better understand the flux emergence processes. Looking forward, we identify open questions regarding magnetic flux emergence that we anticipate can be addressed in the next decade with further observations and simulations.
{"title":"Understanding Active Region Origins and Emergence on the Sun and Other Cool Stars","authors":"Maria A. Weber, Hannah Schunker, Laurène Jouve, Emre Işık","doi":"10.1007/s11214-023-01006-5","DOIUrl":"https://doi.org/10.1007/s11214-023-01006-5","url":null,"abstract":"Abstract The emergence of active regions on the Sun is an integral feature of the solar dynamo mechanism. However, details about the generation of active-region-scale magnetism and the journey of this magnetic flux from the interior to the photosphere are still in question. Shifting paradigms are now developing for the source depth of the Sun’s large-scale magnetism, the organization of this magnetism into fibril flux tubes, and the role of convection in shaping active-region observables. Here we review the landscape of flux emergence theories and simulations, highlight the role flux emergence plays in the global dynamo process, and make connections between flux emergence on the Sun and other cool stars. As longer-term and higher fidelity observations of both solar active regions and their associated flows are amassed, it is now possible to place new constraints on models of emerging flux. We discuss the outcomes of statistical studies which provide observational evidence that flux emergence may be a more passive process (at least in the upper convection zone); dominated to a greater extent by the influence of convection and to a lesser extent by buoyancy and the Coriolis force acting on rising magnetic flux tubes than previously thought. We also discuss how the relationship between stellar rotation, fractional convection zone depth, and magnetic activity on other stars can help us better understand the flux emergence processes. Looking forward, we identify open questions regarding magnetic flux emergence that we anticipate can be addressed in the next decade with further observations and simulations.","PeriodicalId":21902,"journal":{"name":"Space Science Reviews","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-10-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135943958","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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