{
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"page_type": "Visualization",
"title": "Parker Solar Probe: Crossing the Alfven Surface",
"description": "Split window view illustrating the orbit of Parker with the orbit trail colored based on the Mach number of the solar wind and the magnetic field lines (represented as gold) connecting back to the Sun. The Mach number drops below unity (one) when a field line transitions between two different coronal hole regions (the blue and red regions marked on the Sun). || Parker_SolarCloseup.combo.HD1080.00480_print.jpg (1024x576) [121.9 KB] || Parker_SolarCloseup.combo.HD1080.00480_searchweb.png (320x180) [74.1 KB] || Parker_SolarCloseup.combo.HD1080.00480_thm.png (80x40) [5.2 KB] || Parker_SolarCloseup.combo.HD1080 (1920x1080) [0 Item(s)] || Parker_SolarCloseup.combo.HD1080_p30.mp4 (1920x1080) [45.8 MB] || Parker_SolarCloseup.combo.HD1080_p30.webm (1920x1080) [5.6 MB] || Parker_SolarCloseup.combo.UHD2160 (3840x2160) [0 Item(s)] || Parker_SolarCloseup.combo.UHD2160_p30.mp4 (3840x2160) [124.5 MB] || Parker_SolarCloseup.combo.HD1080_p30.mp4.hwshow [202 bytes] || ",
"release_date": "2021-12-14T12:00:00-05:00",
"update_date": "2025-01-06T00:19:29.717640-05:00",
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"alt_text": "Split window view illustrating the orbit of Parker with the orbit trail colored based on the Mach number of the solar wind and the magnetic field lines (represented as gold) connecting back to the Sun. The Mach number drops below unity (one) when a field line transitions between two different coronal hole regions (the blue and red regions marked on the Sun).",
"width": 1024,
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"main_credits": {
"Visualizations by": [
{
"name": "Tom Bridgman",
"employer": "Global Science and Technology, Inc."
}
],
"Scientific consulting by": [
{
"name": "Justin Kasper",
"employer": "University of Michigan"
}
]
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"progress": "Complete",
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"description": "The Sun's corona extends far beyond the solar surface, or photosphere and is considered the outer boundary of the Sun. It marks the transition to the solar wind which moves through the solar system. This limit is defined by the distance at which disturbances in the solar wind cannot propagate back to the solar surface. Those disturbances cannot propagate back towards the Sun if the outbound solar wind speed exceeds Mach one, the speed of 'sound' as defined for the solar wind. This distance forms an irregular 'surface' around the Sun called the Alfvén surface.
Parker Solar Probe has now reached close enough to the Sun that it has begun to penetrate this Alfvén surface. From measurements of the solar wind plasma environment by the Parker's FIELDS and SWEAP instruments, scientists can compute the 'speed of sound' for the plasma, which exhibits brief periods when the Mach number drops below unity (one).
At Parker's distance during encounter 8, the Mach number dropped below unity on several occasions. Propagating the magnetic field vector at Parker back to the solar photosphere revealed that these regions corresponded to significant changes in the magnetic field on the photosphere, particularly that fields lines of 'open' magnetic flux were transitioning from one location to another.
In the visualizations below, we see the measured Mach number at Parker propagated along the orbit, with green representing Mach number greater than one, grey represents Mach number approximately one, and red represents Mach number less than one. When we trace the field lines at these moments back to the Sun, we see the field line jumping between isolated regions of 'open' magnetic flux - blue for inward magnetic flux and red for outbound magnetic flux.",
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"description": "A visualization illustrating the orbit of Parker, orbit trail colored based on the Mach number of the solar wind, with the magnetic field lines (represented in gold) connecting back to the Sun. The Mach number drops below unity (one) when a field line transitions between two different coronal hole regions (the blue and red regions marked on the Sun).",
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"alt_text": "A visualization illustrating the orbit of Parker, orbit trail colored based on the Mach number of the solar wind, with the magnetic field lines (represented in gold) connecting back to the Sun. The Mach number drops below unity (one) when a field line transitions between two different coronal hole regions (the blue and red regions marked on the Sun).",
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"description": "A visualization illustrating the magnetic field lines connecting Parker Solar Probe back to the Sun. When the Mach number in the solar wind drops below unity (one), the field line (gold) transitions between two different coronal hole regions (the blue and red regions marked on the Sun).",
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"alt_text": "A visualization illustrating the magnetic field lines connecting Parker Solar Probe back to the Sun. When the Mach number in the solar wind drops below unity (one), the field line (gold) transitions between two different coronal hole regions (the blue and red regions marked on the Sun).",
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"alt_text": "A visualization illustrating the magnetic field lines connecting Parker Solar Probe back to the Sun. When the Mach number in the solar wind drops below unity (one), the field line (gold) transitions between two different coronal hole regions (the blue and red regions marked on the Sun).",
"width": 1920,
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"alt_text": "A visualization illustrating the magnetic field lines connecting Parker Solar Probe back to the Sun. When the Mach number in the solar wind drops below unity (one), the field line (gold) transitions between two different coronal hole regions (the blue and red regions marked on the Sun).",
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"alt_text": "A visualization illustrating the magnetic field lines connecting Parker Solar Probe back to the Sun. When the Mach number in the solar wind drops below unity (one), the field line (gold) transitions between two different coronal hole regions (the blue and red regions marked on the Sun).",
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"description": "A top-down view from the ecliptic pole of the orbit of Parker Solar Probe for Encounter 8. FIELDS instrument magnetic vector data are projected from the spacecraft position as arrows. The arrows are deep blue for sunward vectors, deep red for anti-sunward, and in between for directions off from this line. The heliospheric magnetic field lines are the gold lines, representing the propagation of the average field measured at Parker, propagated back to the solar photosphere.",
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"alt_text": "A top-down view from the ecliptic pole of the orbit of Parker Solar Probe for Encounter 8. FIELDS instrument magnetic vector data are projected from the spacecraft position as arrows. The arrows are deep blue for sunward vectors, deep red for anti-sunward, and in between for directions off from this line. The heliospheric magnetic field lines are the gold lines, representing the propagation of the average field measured at Parker, propagated back to the solar photosphere.",
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"alt_text": "A top-down view from the ecliptic pole of the orbit of Parker Solar Probe for Encounter 8. FIELDS instrument magnetic vector data are projected from the spacecraft position as arrows. The arrows are deep blue for sunward vectors, deep red for anti-sunward, and in between for directions off from this line. The heliospheric magnetic field lines are the gold lines, representing the propagation of the average field measured at Parker, propagated back to the solar photosphere.",
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"id": 4957,
"url": "https://svs.gsfc.nasa.gov/4957/",
"page_type": "Visualization",
"title": "Parker Solar Probe: The Origins of Switchbacks",
"description": "Most of the magnetic field measured at Parker during this time is directed sunward (blue field lines and vectors). A switchback occurs when the field changes direction almost 180 degrees for a short period of time. FIELDS instrument magnetic vector data are projected from the spacecraft position as arrows. The arrows are colored deep blue for sunward vectors, deep red for anti-sunward, and in between for directions off from this line. The heliospheric magnetic field lines are represented as gold. || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.clockSlate_EarthTarget.HD1080.00990_print.jpg (1024x576) [114.9 KB] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.clockSlate_EarthTarget.HD1080.00990_searchweb.png (320x180) [71.7 KB] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.clockSlate_EarthTarget.HD1080.00990_thm.png (80x40) [4.5 KB] || Switchbacks20181106A (1920x1080) [0 Item(s)] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.HD1080_p30.mp4 (1920x1080) [25.7 MB] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.HD1080_p30.webm (1920x1080) [4.4 MB] || Switchbacks20181106A (3840x2160) [0 Item(s)] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.UHD3840_2160p30.mp4 (3840x2160) [100.2 MB] || ParkerSP.ChaseCloseupAft.Switchbacks20181106A.FIELDS.HD1080_p30.mp4.hwshow [229 bytes] || ",
"release_date": "2021-12-14T12:00:00-05:00",
"update_date": "2025-01-06T00:19:27.633122-05:00",
"main_image": {
"id": 374848,
"url": "https://svs.gsfc.nasa.gov/vis/a000000/a004900/a004957/BaleSwitchbacks.enc06.top.Overview.FIELDS.field.clockSlate_EarthTarget.HD1080.00690_print.jpg",
"filename": "BaleSwitchbacks.enc06.top.Overview.FIELDS.field.clockSlate_EarthTarget.HD1080.00690_print.jpg",
"media_type": "Image",
"alt_text": "A top-down view from the ecliptic pole of the orbit of Parker Solar Probe for Encounter 6. FIELDS instrument magnetic vector data are projected from the spacecraft position with arrows. The arrows are colored deep blue for sunward vectors, deep red for anti-sunward, and in between for directions off from this line. The heliospheric magnetic field lines are the gold lines, representing the propagation of the average field measured at Parker, propagated back to the solar photosphere.",
"width": 1024,
"height": 576,
"pixels": 589824
}
},
{
"id": 14035,
"url": "https://svs.gsfc.nasa.gov/14035/",
"page_type": "Produced Video",
"title": "AGU 2021 - Major discoveries as NASA’s Parker Solar Probe closes in on the Sun",
"description": "NASA’s Parker Solar Probe has now done what no spacecraft has done before—it has officially touched the Sun. Launched in 2018 to study the Sun’s biggest mysteries, the spacecraft has now grazed the edge of the solar atmosphere and gathered new close-up observations of our star. This is allowing us to see the Sun as never before—including the findings in two new papers, which were presented at AGU, that are helping scientists answer fundamental questions about the Sun.PANELISTSDr. Nicola Fox• Heliophysics Division Director of the Science Mission Directorate at NASA HeadquartersDr. Nour Raouafi• Project Scientist for NASA’s Parker Solar Probe• The Johns Hopkins Applied Physics Laboratory Dr. Justin Kasper• Principal Investigator for Solar Wind Electrons Alphas and Protons (SWEAP) Investigation on Parker Solar Probe • BWX Technologies, Inc., University of MichiganProf. Stuart D. Bale• Principal Investigator for Fields Experiment (FIELDS) on Parker Solar Probe • University of California, Berkeley Dr. Kelly Korreck• Program Scientist at NASA Headquarters• Smithsonian Astrophysical Observatory || ",
"release_date": "2021-12-14T12:00:00-05:00",
"update_date": "2023-05-03T13:43:38.987615-04:00",
"main_image": {
"id": 374572,
"url": "https://svs.gsfc.nasa.gov/vis/a010000/a014000/a014035/ParkerBeauty_HD1080.00300_print.jpg",
"filename": "ParkerBeauty_HD1080.00300_print.jpg",
"media_type": "Image",
"alt_text": "Parker Solar Probe has now “touched the Sun”, passing through the Sun’s outer atmosphere, the corona for the first time in April 2021.Credit: NASA GSFC/CIL/Brian Monroe",
"width": 1024,
"height": 576,
"pixels": 589824
}
},
{
"id": 14036,
"url": "https://svs.gsfc.nasa.gov/14036/",
"page_type": "Produced Video",
"title": "Animation: NASA's Parker Solar Probe Enters Solar Atmosphere",
"description": "For the first time in history, a spacecraft has touched the Sun. NASA’s Parker Solar Probe has now flown through the Sun’s upper atmosphere – the corona – and sampled particles and magnetic fields there. The new milestone marks one major step for Parker Solar Probe and one giant leap for solar science. Just as landing on the Moon allowed scientists to understand how it was formed, touching the very stuff the Sun is made of will help scientists uncover critical information about our closest star and its influence on the solar system. On April 28, 2021, during its eighth flyby of the Sun, Parker Solar Probe encountered the specific magnetic and particle conditions at 18.8 solar radii (8.127 million miles) above the solar surface that told scientists it had crossed the Alfvén critical surface for the first time and finally entered the solar atmosphere.More information here. || ",
"release_date": "2021-12-14T12:00:00-05:00",
"update_date": "2023-05-03T13:43:39.083452-04:00",
"main_image": {
"id": 374694,
"url": "https://svs.gsfc.nasa.gov/vis/a010000/a014000/a014036/Final_PSPAlfvenWave_Version2_NoTransitions_H264.00400_print.jpg",
"filename": "Final_PSPAlfvenWave_Version2_NoTransitions_H264.00400_print.jpg",
"media_type": "Image",
"alt_text": "Parker Solar Probe has now “touched the Sun”, passing through the Sun’s outer atmosphere, the corona for the first time in April 2021. The boundary that marks the edge of the corona is the Alfvén critical surface. Inside that surface (circle at left), plasma is connected to the Sun by waves that travel back and forth to the surface. Beyond it (circle at right), the Sun’s magnetic fields and gravity are too weak to contain the plasma and it becomes the solar wind, racing across the solar system so fast that waves within the wind cannot ever travel fast enough to make it back to the Sun. Credit: NASA/Johns Hopkins APL/Ben Smith",
"width": 1024,
"height": 576,
"pixels": 589824
}
},
{
"id": 20354,
"url": "https://svs.gsfc.nasa.gov/20354/",
"page_type": "Animation",
"title": "Animation: Origins of Switchbacks",
"description": "On recent solar encounters, Parker Solar Probe collected data pinpointing the origin of zig-zag-shaped structures in the solar wind, called switchbacks. The data showed one spot switchbacks originate is at the visible surface of the Sun – the photosphere. By the time it reaches Earth, 93 million miles away, the solar wind is an unrelenting headwind of particles and magnetic fields. But as it escapes the Sun, the solar wind is structured and patchy. In the mid-1990s, the NASA-European Space Agency mission Ulysses flew over the Sun’s poles and discovered a handful of bizarre S-shaped kinks in the solar wind’s magnetic field lines, which detoured charged particles on a zig-zag path as they escaped the Sun. For decades, scientists thought these occasional switchbacks were oddities confined to the Sun’s polar regions. In 2019, at 34 solar radii from the Sun, Parker Solar Probe discovered that switchbacks were not rare, but common in the solar wind. This renewed interest in the features raised new questions: Where are they coming from and how do they form and evolve? Were they forged at the surface of the Sun, or shaped by some process kinking magnetic fields in the solar atmosphere? The new findings, in press at the Astrophysical Journal, finally confirm one origin point near the solar surface. More information here. || ",
"release_date": "2021-12-14T12:00:00-05:00",
"update_date": "2023-05-03T13:43:39.481307-04:00",
"main_image": {
"id": 374501,
"url": "https://svs.gsfc.nasa.gov/vis/a020000/a020300/a020354/Parker_SP_new_results_4K_h264.00736_print.jpg",
"filename": "Parker_SP_new_results_4K_h264.00736_print.jpg",
"media_type": "Image",
"alt_text": "Data from Parker Solar Probe has traced the origin of switchbacks – magnetic zig-zag structures in the solar wind – back to the solar surface. At the surface, magnetic funnels emerge from the photosphere between convection cell structures called supergranules. Switchbacks form inside the funnels and rise into the corona and are pushed out on the solar wind. Credit: NASA GSFC/CIL/Jonathan North",
"width": 1024,
"height": 576,
"pixels": 589824
}
}
],
"sources": [],
"products": [
{
"id": 14045,
"url": "https://svs.gsfc.nasa.gov/14045/",
"page_type": "Produced Video",
"title": "NASA's Parker Solar Probe Touches The Sun For The First Time",
"description": "For the first time in history, a spacecraft has touched the Sun. NASA’s Parker Solar Probe has now flown through the Sun’s upper atmosphere – the corona – and sampled particles and magnetic fields there. The new milestone marks one major step for Parker Solar Probe and one giant leap for solar science. Just as landing on the Moon allowed scientists to understand how it was formed, touching the very stuff the Sun is made of will help scientists uncover critical information about our closest star and its influence on the solar system. More information here. || ",
"release_date": "2021-12-14T12:00:00-05:00",
"update_date": "2023-05-03T13:43:39.325301-04:00",
"main_image": {
"id": 374367,
"url": "https://svs.gsfc.nasa.gov/vis/a010000/a014000/a014045/NHQ_2018_0812_Parker_Solar_Probe_Mission_Launches_to_Touch_the_Sun_-_orig.00400_print.jpg",
"filename": "NHQ_2018_0812_Parker_Solar_Probe_Mission_Launches_to_Touch_the_Sun_-_orig.00400_print.jpg",
"media_type": "Image",
"alt_text": "Launch FootageThe United Launch Alliance Delta IV Heavy rocket launches NASA's Parker Solar Probe to touch the Sun, Sunday, Aug. 12, 2018 from Launch Complex 37 at Cape Canaveral Air Force Station, Florida.Credit: NASA",
"width": 1024,
"height": 576,
"pixels": 589824
}
}
],
"newer_versions": [],
"older_versions": [],
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}