Pub Date : 2024-06-17DOI: 10.1038/s41550-024-02280-1
Although stars and galaxies have developed over time, it seems that supermassive black holes already existed at the ‘cosmic dawn’ of the Universe. Analysis of the mid-infrared spectrum of an early quasar (a quasi-stellar object powered by a black hole) suggests that supermassive black holes and their feeding mechanisms were already completely mature when the Universe was 5% of its present age.
{"title":"JWST confirms that quasars do not evolve across cosmic time","authors":"","doi":"10.1038/s41550-024-02280-1","DOIUrl":"10.1038/s41550-024-02280-1","url":null,"abstract":"Although stars and galaxies have developed over time, it seems that supermassive black holes already existed at the ‘cosmic dawn’ of the Universe. Analysis of the mid-infrared spectrum of an early quasar (a quasi-stellar object powered by a black hole) suggests that supermassive black holes and their feeding mechanisms were already completely mature when the Universe was 5% of its present age.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":null,"pages":null},"PeriodicalIF":12.9,"publicationDate":"2024-06-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141333678","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"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 : 2024-06-17DOI: 10.1038/s41550-024-02273-0
Sarah E. I. Bosman, Javier Álvarez-Márquez, Luis Colina, Fabian Walter, Almudena Alonso-Herrero, Martin J. Ward, Göran Östlin, Thomas R. Greve, Gillian Wright, Arjan Bik, Leindert Boogaard, Karina Caputi, Luca Costantin, Andreas Eckart, Macarena García-Marín, Steven Gillman, Jens Hjorth, Edoardo Iani, Olivier Ilbert, Iris Jermann, Alvaro Labiano, Danial Langeroodi, Florian Peißker, Pierluigi Rinaldi, Martin Topinka, Paul van der Werf, Manuel Güdel, Thomas Henning, Pierre-Olivier Lagage, Tom P. Ray, Ewine F. van Dishoeck, Bart Vandenbussche
The rapid assembly of the first supermassive black holes is an enduring mystery. Until now, it was not known whether quasar ‘feeding’ structures (the ‘hot torus’) could assemble as fast as the smaller-scale quasar structures. We present JWST/MRS (rest-frame infrared) spectroscopic observations of the quasar J1120+0641 at z = 7.0848 (well within the epoch of reionization). The hot torus dust was clearly detected at λrest ≃ 1.3 μm, with a black-body temperature of $${T}_{{{{rm{dust}}}}}=text{1,413.5}_{-7.4}^{+5.7}$$ K, slightly elevated compared to similarly luminous quasars at lower redshifts. Importantly, the supermassive black hole mass of J1120+0641 based on the Hα line (accessible only with JWST), MBH = 1.52 ± 0.17 × 109 M⊙, is in good agreement with previous ground-based rest-frame ultraviolet Mg ii measurements. Comparing the ratios of the Hα, Paα and Paβ emission lines to predictions from a simple one-phase Cloudy model, we find that they are consistent with originating from a common broad-line region with physical parameters that are consistent with lower-redshift quasars. Together, this implies that J1120+0641’s accretion structures must have assembled very quickly, as they appear fully ‘mature’ less than 760 Myr after the Big Bang. A JWST/MIRI spectrum of an early quasar in the mid-infrared indicates that J1120+0641 had a mature feeding structure 760 Myr after the Big Bang. This finding suggests that supermassive black holes and their torii build up surprisingly quickly.
{"title":"A mature quasar at cosmic dawn revealed by JWST rest-frame infrared spectroscopy","authors":"Sarah E. I. Bosman, Javier Álvarez-Márquez, Luis Colina, Fabian Walter, Almudena Alonso-Herrero, Martin J. Ward, Göran Östlin, Thomas R. Greve, Gillian Wright, Arjan Bik, Leindert Boogaard, Karina Caputi, Luca Costantin, Andreas Eckart, Macarena García-Marín, Steven Gillman, Jens Hjorth, Edoardo Iani, Olivier Ilbert, Iris Jermann, Alvaro Labiano, Danial Langeroodi, Florian Peißker, Pierluigi Rinaldi, Martin Topinka, Paul van der Werf, Manuel Güdel, Thomas Henning, Pierre-Olivier Lagage, Tom P. Ray, Ewine F. van Dishoeck, Bart Vandenbussche","doi":"10.1038/s41550-024-02273-0","DOIUrl":"10.1038/s41550-024-02273-0","url":null,"abstract":"The rapid assembly of the first supermassive black holes is an enduring mystery. Until now, it was not known whether quasar ‘feeding’ structures (the ‘hot torus’) could assemble as fast as the smaller-scale quasar structures. We present JWST/MRS (rest-frame infrared) spectroscopic observations of the quasar J1120+0641 at z = 7.0848 (well within the epoch of reionization). The hot torus dust was clearly detected at λrest ≃ 1.3 μm, with a black-body temperature of $${T}_{{{{rm{dust}}}}}=text{1,413.5}_{-7.4}^{+5.7}$$ K, slightly elevated compared to similarly luminous quasars at lower redshifts. Importantly, the supermassive black hole mass of J1120+0641 based on the Hα line (accessible only with JWST), MBH = 1.52 ± 0.17 × 109 M⊙, is in good agreement with previous ground-based rest-frame ultraviolet Mg ii measurements. Comparing the ratios of the Hα, Paα and Paβ emission lines to predictions from a simple one-phase Cloudy model, we find that they are consistent with originating from a common broad-line region with physical parameters that are consistent with lower-redshift quasars. Together, this implies that J1120+0641’s accretion structures must have assembled very quickly, as they appear fully ‘mature’ less than 760 Myr after the Big Bang. A JWST/MIRI spectrum of an early quasar in the mid-infrared indicates that J1120+0641 had a mature feeding structure 760 Myr after the Big Bang. This finding suggests that supermassive black holes and their torii build up surprisingly quickly.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":null,"pages":null},"PeriodicalIF":12.9,"publicationDate":"2024-06-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141333550","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"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 : 2024-06-13DOI: 10.1038/s41550-024-02293-w
David Trang, Christina E. Swafford, Tamar A. Kreps, Steven D. Vance, Jemma Davidson, Justin Filiberto, Lillian R. Ostrach, Christina R. Richey
There is a growing recognition of a mental health crisis within the academic and research communities. Members of the planetary science community have called for healthier work environments to improve mental well-being. As a preliminary step towards improving workplace culture, we sought to determine whether the broader mental health crisis extends to planetary science and to assess the severity of anxiety, depressive and stress symptoms. Our 2022 mental health survey of the planetary science community suggests that the severity of anxiety and depressive symptoms in the community is greater than in the general US population. Furthermore, anxiety and depressive symptoms are more severe for graduate students and postdoctoral researchers than any other career stage. Comparing groups within planetary science, we found that anxiety, depressive and/or stress symptoms appear greater among marginalized groups, such as women, people of colour and members of the LGBTQ+ community. A mental health problem is impacting the planetary science community. Improving well-being will promote enhanced research quality and productivity. Anxiety, depression and stress are significantly more present in the planetary science community than in the general US population. More marginalized demographics, such as sexual and gender minorities, early career researchers, and people of colour or multiracial people, are especially affected.
{"title":"A survey of the severity of mental health symptoms in the planetary science community","authors":"David Trang, Christina E. Swafford, Tamar A. Kreps, Steven D. Vance, Jemma Davidson, Justin Filiberto, Lillian R. Ostrach, Christina R. Richey","doi":"10.1038/s41550-024-02293-w","DOIUrl":"10.1038/s41550-024-02293-w","url":null,"abstract":"There is a growing recognition of a mental health crisis within the academic and research communities. Members of the planetary science community have called for healthier work environments to improve mental well-being. As a preliminary step towards improving workplace culture, we sought to determine whether the broader mental health crisis extends to planetary science and to assess the severity of anxiety, depressive and stress symptoms. Our 2022 mental health survey of the planetary science community suggests that the severity of anxiety and depressive symptoms in the community is greater than in the general US population. Furthermore, anxiety and depressive symptoms are more severe for graduate students and postdoctoral researchers than any other career stage. Comparing groups within planetary science, we found that anxiety, depressive and/or stress symptoms appear greater among marginalized groups, such as women, people of colour and members of the LGBTQ+ community. A mental health problem is impacting the planetary science community. Improving well-being will promote enhanced research quality and productivity. Anxiety, depression and stress are significantly more present in the planetary science community than in the general US population. More marginalized demographics, such as sexual and gender minorities, early career researchers, and people of colour or multiracial people, are especially affected.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":null,"pages":null},"PeriodicalIF":12.9,"publicationDate":"2024-06-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141319813","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"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}
Rotation is an intrinsic property of stars and provides essential constraints on their structure, formation, evolution and interaction with the interplanetary environment. The Sun provides a unique opportunity to explore stellar rotation from the interior to its atmosphere in great detail. We know that the Sun rotates faster at the equator than at the poles, but how this differential rotation behaves at different atmospheric layers within it is not yet clear. Here we extract the rotation curves of different layers of the solar photosphere and chromosphere by using whole-disk Dopplergrams obtained by the Chinese Hα Solar Explorer (CHASE) for the wavebands Si i (6,560.58 Å), Hα (6,562.81 Å) and Fe i (6,569.21 Å) with a spectral resolution of 0.024 Å. We find that the Sun rotates progressively faster from the photosphere to the chromosphere. For example, at the equator, it increases from 2.81 ± 0.02 μrad s−1 at the bottom of the photosphere to 3.08 ± 0.05 μrad s−1 in the chromosphere. The ubiquitous small-scale magnetic fields and the height-dependent degree of their frozen-in effect with the solar atmosphere are plausible causes of the height-dependent rotation rate. The results have important implications for understanding solar subsurface processes and solar atmospheric dynamics.
{"title":"Height-dependent differential rotation of the solar atmosphere detected by CHASE","authors":"Shihao Rao, Chuan Li, Mingde Ding, Jie Hong, Feng Chen, Cheng Fang, Ye Qiu, Zhen Li, Pengfei Chen, Kejun Li, Qi Hao, Yang Guo, Xin Cheng, Yu Dai, Zhixin Peng, Wei You, Yuan Yuan","doi":"10.1038/s41550-024-02299-4","DOIUrl":"https://doi.org/10.1038/s41550-024-02299-4","url":null,"abstract":"<p>Rotation is an intrinsic property of stars and provides essential constraints on their structure, formation, evolution and interaction with the interplanetary environment. The Sun provides a unique opportunity to explore stellar rotation from the interior to its atmosphere in great detail. We know that the Sun rotates faster at the equator than at the poles, but how this differential rotation behaves at different atmospheric layers within it is not yet clear. Here we extract the rotation curves of different layers of the solar photosphere and chromosphere by using whole-disk Dopplergrams obtained by the Chinese Hα Solar Explorer (CHASE) for the wavebands Si <span>i</span> (6,560.58 Å), Hα (6,562.81 Å) and Fe <span>i</span> (6,569.21 Å) with a spectral resolution of 0.024 Å. We find that the Sun rotates progressively faster from the photosphere to the chromosphere. For example, at the equator, it increases from 2.81 ± 0.02 μrad s<sup>−1</sup> at the bottom of the photosphere to 3.08 ± 0.05 μrad s<sup>−1</sup> in the chromosphere. The ubiquitous small-scale magnetic fields and the height-dependent degree of their frozen-in effect with the solar atmosphere are plausible causes of the height-dependent rotation rate. The results have important implications for understanding solar subsurface processes and solar atmospheric dynamics.</p>","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":null,"pages":null},"PeriodicalIF":14.1,"publicationDate":"2024-06-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141319985","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"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 : 2024-06-10DOI: 10.1038/s41550-024-02279-8
Merav Opher, Abraham Loeb, J. E. G. Peek
Cold, dense clouds in the interstellar medium of our Galaxy are 4–5 orders of magnitude denser than their diffuse counterparts. Our Solar System has most likely encountered at least one of these dense clouds during its lifetime. However, evidence for such an encounter has not been studied in detail yet. Here we derive the velocity field of the Local Ribbon of Cold Clouds (LRCC) by modelling the 21 cm data from the HI4PI survey, finding that the Solar System may have passed through the LRCC in the constellation Lynx 2–3 million years ago. Using a state-of-the-art simulation of the heliosphere, we show that during the passage, the heliosphere shrinks to a scale of 0.22 au, smaller than the Earth’s orbit around the Sun. This would have put the Earth in direct contact with the dense interstellar medium for a period of time and exposed it to a neutral hydrogen density above 3,000 cm−3. Such a scenario agrees with geological evidence from 60Fe and 244Pu isotopes. The encounter and related increased radiation from Galactic cosmic rays might have had a substantial impact on the Earth’s system and climate. Modelling suggests that the Solar System may have passed through a cold dense cloud 2–3 Myr ago, in agreement with geological evidence from 60Fe and 244Pu isotopes, putting Earth in direct contact with the dense interstellar medium with potentially substantial impacts on its climate.
{"title":"A possible direct exposure of the Earth to the cold dense interstellar medium 2–3 Myr ago","authors":"Merav Opher, Abraham Loeb, J. E. G. Peek","doi":"10.1038/s41550-024-02279-8","DOIUrl":"10.1038/s41550-024-02279-8","url":null,"abstract":"Cold, dense clouds in the interstellar medium of our Galaxy are 4–5 orders of magnitude denser than their diffuse counterparts. Our Solar System has most likely encountered at least one of these dense clouds during its lifetime. However, evidence for such an encounter has not been studied in detail yet. Here we derive the velocity field of the Local Ribbon of Cold Clouds (LRCC) by modelling the 21 cm data from the HI4PI survey, finding that the Solar System may have passed through the LRCC in the constellation Lynx 2–3 million years ago. Using a state-of-the-art simulation of the heliosphere, we show that during the passage, the heliosphere shrinks to a scale of 0.22 au, smaller than the Earth’s orbit around the Sun. This would have put the Earth in direct contact with the dense interstellar medium for a period of time and exposed it to a neutral hydrogen density above 3,000 cm−3. Such a scenario agrees with geological evidence from 60Fe and 244Pu isotopes. The encounter and related increased radiation from Galactic cosmic rays might have had a substantial impact on the Earth’s system and climate. Modelling suggests that the Solar System may have passed through a cold dense cloud 2–3 Myr ago, in agreement with geological evidence from 60Fe and 244Pu isotopes, putting Earth in direct contact with the dense interstellar medium with potentially substantial impacts on its climate.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":null,"pages":null},"PeriodicalIF":12.9,"publicationDate":"2024-06-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.nature.com/articles/s41550-024-02279-8.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141304541","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-06-06DOI: 10.1038/s41550-024-02288-7
What drives the solar wind complexity and variability seen in the heliosphere remains an unresolved mystery. Unique high-resolution observations and measurements taken at 0.5 au, coupled with magnetic modelling and spectroscopic techniques, show that the variability is driven by spatio-temporal changes in the magnetic connectivity to multiple solar source regions.
太阳风在日光层中的复杂性和可变性的驱动因素仍然是一个未解之谜。在 0.5 au 处进行的独特的高分辨率观测和测量，以及磁建模和光谱技术表明，这种变化是由与多个太阳源区的磁连接的时空变化驱动的。
{"title":"High-resolution observations and measurements show variability of multi-source solar wind","authors":"","doi":"10.1038/s41550-024-02288-7","DOIUrl":"10.1038/s41550-024-02288-7","url":null,"abstract":"What drives the solar wind complexity and variability seen in the heliosphere remains an unresolved mystery. Unique high-resolution observations and measurements taken at 0.5 au, coupled with magnetic modelling and spectroscopic techniques, show that the variability is driven by spatio-temporal changes in the magnetic connectivity to multiple solar source regions.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":null,"pages":null},"PeriodicalIF":12.9,"publicationDate":"2024-06-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141264719","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"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 : 2024-06-05DOI: 10.1038/s41550-024-02277-w
M. Caleb, E. Lenc, D. L. Kaplan, T. Murphy, Y. P. Men, R. M. Shannon, L. Ferrario, K. M. Rajwade, T. E. Clarke, S. Giacintucci, N. Hurley-Walker, S. D. Hyman, M. E. Lower, Sam McSweeney, V. Ravi, E. D. Barr, S. Buchner, C. M. L. Flynn, J. W. T. Hessels, M. Kramer, J. Pritchard, B. W. Stappers
Long-period radio transients are an emerging class of extreme astrophysical events of which only three are known. These objects emit highly polarized, coherent pulses of typically a few tens of seconds duration, and minutes to approximately hour-long periods. Although magnetic white dwarfs and magnetars, either isolated or in binary systems, have been invoked to explain these objects, a consensus has not emerged. Here we report on the discovery of ASKAP J193505.1+214841.0 (henceforth ASKAP J1935+2148) with a period of 53.8 minutes showing 3 distinct emission states—a bright pulse state with highly linearly polarized pulses with widths of 10–50 seconds; a weak pulse state that is about 26 times fainter than the bright state with highly circularly polarized pulses of widths of approximately 370 milliseconds; and a quiescent or quenched state with no pulses. The first two states have been observed to progressively evolve over the course of 8 months with the quenched state interspersed between them suggesting physical changes in the region producing the emission. A constraint on the radius of the source for the observed period rules out an isolated magnetic white-dwarf origin. Unlike other long-period sources, ASKAP 1935+2148 shows marked variations in emission modes reminiscent of neutron stars. However, its radio properties challenge our current understanding of neutron-star emission and evolution.
{"title":"An emission-state-switching radio transient with a 54-minute period","authors":"M. Caleb, E. Lenc, D. L. Kaplan, T. Murphy, Y. P. Men, R. M. Shannon, L. Ferrario, K. M. Rajwade, T. E. Clarke, S. Giacintucci, N. Hurley-Walker, S. D. Hyman, M. E. Lower, Sam McSweeney, V. Ravi, E. D. Barr, S. Buchner, C. M. L. Flynn, J. W. T. Hessels, M. Kramer, J. Pritchard, B. W. Stappers","doi":"10.1038/s41550-024-02277-w","DOIUrl":"https://doi.org/10.1038/s41550-024-02277-w","url":null,"abstract":"<p>Long-period radio transients are an emerging class of extreme astrophysical events of which only three are known. These objects emit highly polarized, coherent pulses of typically a few tens of seconds duration, and minutes to approximately hour-long periods. Although magnetic white dwarfs and magnetars, either isolated or in binary systems, have been invoked to explain these objects, a consensus has not emerged. Here we report on the discovery of ASKAP J193505.1+214841.0 (henceforth ASKAP J1935+2148) with a period of 53.8 minutes showing 3 distinct emission states—a bright pulse state with highly linearly polarized pulses with widths of 10–50 seconds; a weak pulse state that is about 26 times fainter than the bright state with highly circularly polarized pulses of widths of approximately 370 milliseconds; and a quiescent or quenched state with no pulses. The first two states have been observed to progressively evolve over the course of 8 months with the quenched state interspersed between them suggesting physical changes in the region producing the emission. A constraint on the radius of the source for the observed period rules out an isolated magnetic white-dwarf origin. Unlike other long-period sources, ASKAP 1935+2148 shows marked variations in emission modes reminiscent of neutron stars. However, its radio properties challenge our current understanding of neutron-star emission and evolution.</p>","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":null,"pages":null},"PeriodicalIF":14.1,"publicationDate":"2024-06-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141251654","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"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 : 2024-05-30DOI: 10.1038/s41550-024-02297-6
Ryan M. Lau, Amit Ashok, Julie Emms, Douglas R. Gies, Saikat Guha, Zachary Hartman, Brittany McClinton, John Monnier, Jayadev K. Rajagopal, J. Gabriel Richardson, Stephen T. Ridgway, Joel Sanchez-Bermudez, Gail Schaefer, Brian J. Smith, Aziza Suleymanzade
The astronomy and quantum information science communities met together in a one-day workshop to share experiences and ideas on how to reach the next level — the quantum level — of astronomical interferometry.
{"title":"Charting quantum horizons to establish a roadmap for microsecond astronomy","authors":"Ryan M. Lau, Amit Ashok, Julie Emms, Douglas R. Gies, Saikat Guha, Zachary Hartman, Brittany McClinton, John Monnier, Jayadev K. Rajagopal, J. Gabriel Richardson, Stephen T. Ridgway, Joel Sanchez-Bermudez, Gail Schaefer, Brian J. Smith, Aziza Suleymanzade","doi":"10.1038/s41550-024-02297-6","DOIUrl":"10.1038/s41550-024-02297-6","url":null,"abstract":"The astronomy and quantum information science communities met together in a one-day workshop to share experiences and ideas on how to reach the next level — the quantum level — of astronomical interferometry.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":null,"pages":null},"PeriodicalIF":12.9,"publicationDate":"2024-05-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141177285","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"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 : 2024-05-28DOI: 10.1038/s41550-024-02278-9
Stephanie L. Yardley, David H. Brooks, Raffaella D’Amicis, Christopher J. Owen, David M. Long, Deb Baker, Pascal Démoulin, Mathew J. Owens, Mike Lockwood, Teodora Mihailescu, Jesse T. Coburn, Ryan M. Dewey, Daniel Müller, Gabriel H. H. Suen, Nawin Ngampoopun, Philippe Louarn, Stefano Livi, Sue Lepri, Andrzej Fludra, Margit Haberreiter, Udo Schühle
The ambient solar wind that fills the heliosphere originates from multiple sources in the solar corona and is highly structured. It is often described as high-speed, relatively homogeneous, plasma streams from coronal holes and slow-speed, highly variable, streams whose source regions are under debate. A key goal of ESA/NASA’s Solar Orbiter mission is to identify solar wind sources and understand what drives the complexity seen in the heliosphere. By combining magnetic field modelling and spectroscopic techniques with high-resolution observations and measurements, we show that the solar wind variability detected in situ by Solar Orbiter in March 2022 is driven by spatio-temporal changes in the magnetic connectivity to multiple sources in the solar atmosphere. The magnetic field footpoints connected to the spacecraft moved from the boundaries of a coronal hole to one active region (12961) and then across to another region (12957). This is reflected in the in situ measurements, which show the transition from fast to highly Alfvénic then to slow solar wind that is disrupted by the arrival of a coronal mass ejection. Our results describe solar wind variability at 0.5 au but are applicable to near-Earth observatories. Solar wind is highly structured yet variable. Close-up observations of the solar atmosphere reveal that the changing connectivity of multiple sources in the solar corona drives the observed complexity and variability in the inner heliosphere.
填充日光层的环境太阳风来自日冕的多个源头，结构非常复杂。它通常被描述为来自日冕洞的高速、相对均匀的等离子体流和慢速、高度可变的等离子体流，其来源区域还在争论之中。欧空局/美国国家航空航天局太阳轨道飞行器任务的一个关键目标是确定太阳风的来源，了解日光层复杂性的驱动因素。通过将磁场建模和光谱技术与高分辨率观测和测量相结合，我们表明太阳轨道器在2022年3月现场探测到的太阳风变化是由与太阳大气中多个来源的磁连接的时空变化驱动的。与航天器相连的磁场脚点从日冕洞的边界移动到一个活跃区域（12961），然后又横跨到另一个区域（12957）。这反映在现场测量中，显示了太阳风从快速到高阿尔费尼，再到慢速的过渡，而日冕物质抛射的到来又扰乱了这一过渡。我们的结果描述了 0.5 au 太阳风的变化，但适用于近地观测站。
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