STEVE

Last updated
A STEVE over Little Bow Resort, Alberta, in August 2015 Optical Steve.jpg
A STEVE over Little Bow Resort, Alberta, in August 2015
A STEVE over Crossfield, Alberta, in March 2018 (around 12:30 a.m.) The Aurora Named STEVE (26938621998).jpg
A STEVE over Crossfield, Alberta, in March 2018 (around 12:30 a.m.)

STEVE is an atmospheric optical phenomenon that appears as a purple and green light ribbon in the night sky, named in late 2016 by aurora watchers from Alberta, Canada. The backronym later adopted for the phenomenon is the Strong Thermal Emission Velocity Enhancement. According to analysis of satellite data from the European Space Agency's Swarm mission, the phenomenon is caused by a 25 km (16 mi) wide ribbon of hot plasma at an altitude of 450 km (280 mi), with a temperature of 3,000 °C (3,270 K; 5,430 °F) and flowing at a speed of 6 km/s (3.7 mi/s) (compared to 10 m/s (33 ft/s) outside the ribbon). The phenomenon is not rare, but had not been investigated and described scientifically prior to that time. [1] [2] [3]

Contents

Discovery and naming

The STEVE phenomenon has been observed by auroral photographers for decades. [3] Some evidence suggests that STEVE observations may have been recorded as early as 1705. [4] Notations resembling the phenomenon exist in some observations from 1911 to the 1950s by Carl Størmer. [5] [6]

The first accurate determination of the nature of the phenomenon was not made, however, until after members of a Facebook group, Alberta Aurora Chasers, named it, attributed it to a proton aurora, and began calling it a "proton arc". [7] When physics professor Eric Donovan from the University of Calgary saw their photographs and suspected that their determination was incorrect because proton auroras are not visible, [8] he correlated the time and location of the phenomenon with Swarm satellite data and one of the Alberta Aurora Chaser photographers, Song Despins. She provided GPS coordinates from Vimy, Alberta, that helped Donovan link the data to identify the phenomenon. [1]

One of the aurora watchers, photographer Chris Ratzlaff, [9] [10] suggested using the name "Steve" for the phenomenon, in reference to Over the Hedge, an animated comedy movie from 2006. The characters in the movie give the name to a hedge that appears overnight, in order to make it seem more benign. [11] Reports of the heretofore undescribed and unusual "aurora" went viral as an example of citizen science on Aurorasaurus. [12] [13]

During the fall meeting of the American Geophysical Union in December 2016, Robert Lysak suggested using a backronym of "Steve" for the phenomenon that would stand for a "Strong Thermal Emission Velocity Enhancement". [14] That acronym, "STEVE", has been adopted by the team at NASA Goddard Space Flight Center that is studying the phenomenon. [15]

External media
Images
Searchtool.svg Photograph of the phenomenon
Searchtool.svg Gallery
Video
Nuvola apps kaboodle.svg Time-lapse phenomenon on YouTube

Occurrence and cause

Location and timing

STEVE phenomena may be spotted further from the poles than the aurora, [16] and as of March 2018, have been observed in the United Kingdom, Canada, Alaska, northern U.S. states, Australia, New Zealand [17] and Denmark. [18] The phenomenon appears as a very narrow arc extending for hundreds or thousands of kilometers, aligned east–west. It generally lasts for twenty minutes to an hour. As of March 2018, STEVE phenomena have only been spotted in the presence of an aurora. None were observed from October 2016 to February 2017, or from October 2017 to February 2018, leading NASA to believe that STEVE phenomena may only appear during certain seasons. [19] However, STEVE phenomena have since been reported and photographed in South Australia during a geomagnetic storm event on 11 October 2024. [20]

Research into cause

A study published in March 2018 by Elizabeth A. MacDonald and co-authors in the peer-reviewed journal, Science Advances , suggested that the STEVE phenomenon accompanies a subauroral ion drift (SAID), [21] a fast-moving stream of extremely hot particles. STEVE marks the first observed visual effect accompanying a SAID. [19]

In August 2018, researchers determined that the skyglow of the phenomenon was not associated with particle precipitation (electrons or ions) and, as a result, could be generated in the ionosphere. [22]

One proposed mechanism for the glow is that excited nitrogen breaks apart and interacts with oxygen to form glowing nitric oxide. [23]

Association with picket-fence aurora

Often, although not always, a STEVE phenomenon is observed above a green, "picket-fence" aurora according to a study published in Geophysical Research Letters. [24] [25] Although the picket-fence aurora is created through precipitation of electrons, they appear outside the auroral oval and so their formation is different from traditional aurora. [26] The study also showed these phenomena appear in both hemispheres simultaneously. Sightings of picket-fence aurora have been made without observations of STEVE. [27]

The green emissions in the picket fence aurora seem to be related to eddies in the supersonic flow of charged particles, similar to the eddies seen in a river that move more slowly than the water around them. Hence, the green bars in the picket fence are moving more slowly than the structures in the purple emissions and some scientists have speculated they could be caused by turbulence in the charged particles from space. [28]

Research

2017

2018

2019

2020

2021

2022

2023

See also

Related Research Articles

<span class="mw-page-title-main">Aurora</span> Atmospheric effect caused by the solar wind

An aurora , also commonly known as the northern lights or southern lights, is a natural light display in Earth's sky, predominantly seen in high-latitude regions. Auroras display dynamic patterns of brilliant lights that appear as curtains, rays, spirals, or dynamic flickers covering the entire sky.

<span class="mw-page-title-main">High-frequency Active Auroral Research Program</span> Project to analyze the ionosphere

The High-frequency Active Auroral Research Program (HAARP) is a University of Alaska Fairbanks program which researches the ionosphere – the highest, ionized part of Earth's atmosphere. The most prominent instrument at HAARP is the Ionospheric Research Instrument (IRI), a high-power radio frequency transmitter facility operating in the high frequency (HF) band. The IRI is used to temporarily excite a limited area of the ionosphere. Other instruments, such as a VHF and a UHF radar, a fluxgate magnetometer, a digisonde, and an induction magnetometer, are used to study the physical processes that occur in the excited region. Work on the HAARP facility began in 1993. Initially HAARP was jointly funded by the U.S. Air Force, the U.S. Navy, the University of Alaska Fairbanks, and the Defense Advanced Research Projects Agency (DARPA). It was designed and built by BAE Advanced Technologies. Its original purpose was to analyze the ionosphere and investigate the potential for developing ionospheric enhancement technology for radio communications and surveillance. Since 2015 it has been operated by the University of Alaska Fairbanks.

<span class="mw-page-title-main">Whistler (radio)</span> Very low frequency EM waves generated by lightning

A whistler is a very low frequency (VLF) electromagnetic (radio) wave generated by lightning. Frequencies of terrestrial whistlers are 1 kHz to 30 kHz, with maximum frequencies usually at 3 kHz to 5 kHz. Although they are electromagnetic waves, they occur at audio frequencies, and can be converted to audio using a suitable receiver. They are produced by lightning strikes where the impulse travels along the Earth's magnetic field lines from one hemisphere to the other. They undergo dispersion of several kHz due to the slower velocity of the lower frequencies through the plasma environments of the ionosphere and magnetosphere. Thus they are perceived as a descending tone which can last for a few seconds. The study of whistlers categorizes them into Pure Note, Diffuse, 2-Hop, and Echo Train types.

<span class="mw-page-title-main">Magnetosphere of Saturn</span> Cavity in the solar wind the sixth planet creates

The magnetosphere of Saturn is the cavity created in the flow of the solar wind by the planet's internally generated magnetic field. Discovered in 1979 by the Pioneer 11 spacecraft, Saturn's magnetosphere is the second largest of any planet in the Solar System after Jupiter. The magnetopause, the boundary between Saturn's magnetosphere and the solar wind, is located at a distance of about 20 Saturn radii from the planet's center, while its magnetotail stretches hundreds of Saturn radii behind it.

<span class="mw-page-title-main">Cluster II (spacecraft)</span> European Space Agency space mission

Cluster II was a space mission of the European Space Agency, with NASA participation, to study the Earth's magnetosphere over the course of nearly two solar cycles. The mission was composed of four identical spacecraft flying in a tetrahedral formation. As a replacement for the original Cluster spacecraft which were lost in a launch failure in 1996, the four Cluster II spacecraft were successfully launched in pairs in July and August 2000 onboard two Soyuz-Fregat rockets from Baikonur, Kazakhstan. In February 2011, Cluster II celebrated 10 years of successful scientific operations in space. In February 2021, Cluster II celebrated 20 years of successful scientific operations in space. As of March 2023, its mission was extended until September 2024. The China National Space Administration/ESA Double Star mission operated alongside Cluster II from 2004 to 2007.

<span class="mw-page-title-main">Birkeland current</span> Currents flowing along geomagnetic field lines

A Birkeland current is a set of electrical currents that flow along geomagnetic field lines connecting the Earth's magnetosphere to the Earth's high latitude ionosphere. In the Earth's magnetosphere, the currents are driven by the solar wind and interplanetary magnetic field (IMF) and by bulk motions of plasma through the magnetosphere. The strength of the Birkeland currents changes with activity in the magnetosphere. Small scale variations in the upward current sheets accelerate magnetospheric electrons which, when they reach the upper atmosphere, create the Auroras Borealis and Australis.

Ashen light is a hypothesised subtle glow that has been claimed to be seen on the night side of the planet Venus. The phenomenon has not been scientifically confirmed, and theories as to the observed phenomenon's cause are numerous, such as emission of light by Venus, or optical phenomena within the observing telescope itself. A modern hypothesis as to the source of light on Venus suggests it to be associated with lightning, for which there is some evidence on Venus. This theory has fallen out of favour, however, as there is not enough light generated by this lightning so as to be observed. A more recent hypothesis is that it is a form of transient aurorae or airglow caused by unusually high solar activity interacting with the upper Venusian atmosphere.

<span class="mw-page-title-main">Magnetosphere of Jupiter</span> Cavity created in the solar wind

The magnetosphere of Jupiter is the cavity created in the solar wind by Jupiter's magnetic field. Extending up to seven million kilometers in the Sun's direction and almost to the orbit of Saturn in the opposite direction, Jupiter's magnetosphere is the largest and most powerful of any planetary magnetosphere in the Solar System, and by volume the largest known continuous structure in the Solar System after the heliosphere. Wider and flatter than the Earth's magnetosphere, Jupiter's is stronger by an order of magnitude, while its magnetic moment is roughly 18,000 times larger. The existence of Jupiter's magnetic field was first inferred from observations of radio emissions at the end of the 1950s and was directly observed by the Pioneer 10 spacecraft in 1973.

<span class="mw-page-title-main">Canadian Geospace Monitoring</span> Canadian space science program

Canadian Geospace Monitoring (CGSM) is a Canadian space science program that was initiated in 2005. CGSM is funded primarily by the Canadian Space Agency, and consists of networks of imagers, meridian scanning photometers, riometers, magnetometers, digital ionosondes, and High Frequency SuperDARN radars. The overarching objective of CGSM is to provide synoptic observations of the spatio-temporal evolution of the ionospheric thermodynamics and electrodynamics at auroral and polar latitudes over a large region of Canada.

A double layer is a structure in a plasma consisting of two parallel layers of opposite electrical charge. The sheets of charge, which are not necessarily planar, produce localised excursions of electric potential, resulting in a relatively strong electric field between the layers and weaker but more extensive compensating fields outside, which restore the global potential. Ions and electrons within the double layer are accelerated, decelerated, or deflected by the electric field, depending on their direction of motion.

<span class="mw-page-title-main">Substorm</span> Short term magnetosphere disturbance

A substorm, sometimes referred to as a magnetospheric substorm or an auroral substorm, is a brief disturbance in the Earth's magnetosphere that causes energy to be released from the "tail" of the magnetosphere and injected into the high latitude ionosphere. Visually, a substorm is seen as a sudden brightening and increased movement of auroral arcs. Substorms were first described in qualitative terms by Kristian Birkeland which he called polar elementary storms. Sydney Chapman used the term substorm about 1960 which is now the standard term. The morphology of aurora during a substorm was first described by Syun-Ichi Akasofu in 1964 using data collected during the International Geophysical Year.

<span class="mw-page-title-main">SMILE (spacecraft)</span> Chinese–European satellite studying Earths magnetosphere

Solar wind Magnetosphere Ionosphere Link Explorer (SMILE) is a planned joint venture mission between the European Space Agency and the Chinese Academy of Sciences. SMILE will image for the first time the magnetosphere of the Sun in soft X-rays and UV during up to 40 hours per orbit, improving our understanding of the dynamic interaction between the solar wind and Earth's magnetosphere. The prime science questions of the SMILE mission are

<span class="mw-page-title-main">Gordon G. Shepherd</span> Canadian space scientist

Gordon Greeley Shepherd is a Canadian space scientist, currently a Distinguished Research Professor Emeritus at York University

<span class="mw-page-title-main">Liz MacDonald</span> American space weather scientist

Elizabeth MacDonald is a space weather scientist who works at NASA Goddard Space Flight Center. She is a co-investigator on the Helium, Oxygen, Proton, and Electron Spectrometer on the NASA Radiation Belts Storm Probe mission.

<span class="mw-page-title-main">John Bird (scientist)</span> Canadian engineer

John Clifford Bird is a Canadian engineer, scientist, and journalist. Bird’s research has included laser physics, atmospheric physics, and materials in microgravity. He broke the world altitude record for hang gliding by launching from a helium balloon at 35,000 ft, and spent a year at the Amundsen–Scott South Pole Station, which was documented in his book One Day, One Night: Portraits of the South Pole.

A subauroral ion drift (SAID), also known as a polarisation jet, is an atmospheric phenomenon driven by substorms in the Earth's magnetosphere. First discovered in 1971, a SAID is a latitudinally narrow layer of rapid, westward flowing ions in the Earth’s ionosphere. Though not traditionally associated with an optical emission, the STEVE discovery paper suggested the first link between this optical emission’s occurrence and that of an extremely fast and hot SAID event.

Cynthia Cattell is a space plasma physicist known for her research on solar flares and radiation belts.

Michael Mendillo is a professor of astronomy at Boston University. His primary research interests include space physics, planetary atmospheres, observations and models. He is a Fellow of the American Geophysical Union and a longtime member of the American Astronomical Society.

<span class="mw-page-title-main">James Dungey</span> British space scientist

James Wynne Dungey (1923–2015) was a British space scientist who was pivotal in establishing the field of space weather and made significant contributions to the fundamental understanding of plasma physics.

References

  1. 1 2 McRae, Mike (24 April 2017). "Introducing Steve - a Newly Discovered Astronomical Phenomenon". ScienceAlert .
  2. ↑ "When Swarm Met Steve". esa.int. European Space Agency. 21 April 2017.
  3. 1 2 "New kind of aurora is not an aurora at all". American Geophysical Union. 20 August 2018. Retrieved 2018-08-21– via Phys.org.
  4. ↑ Finnegan, James; Asher, David; Nezic, Rok; Byrne, Conor; Bailey, Mark (23 July 2018). "Historical observations of STEVE". The Observatory. 138: 227–245. arXiv: 1808.01872 . Bibcode:2018Obs...138..227B.
  5. ↑ Hunnekuhl M, MacDonald E (12 February 2020). "Early Ground-Based Work by Auroral Pioneer Carl Størmer on the High-Altitude Detached Subauroral Arcs Now Known as "STEVE"". Space Weather. 18 (3). Bibcode:2020SpWea..1802384H. doi: 10.1029/2019SW002384 .
  6. ↑ "When Størmer Met STEVE". Aurorasaurus. 3 March 2020.
  7. ↑ "Meet Steve". European Space Agency. Retrieved 2017-04-24.
  8. ↑ "Aurora photographers find new night sky lights and call them Steve". BBC News. 23 April 2017.
  9. ↑ ""I propose we call it Steve until then" - Alberta Aurora Chasers". Facebook . February 10, 2016.
  10. ↑ "Amateur Sky-Watchers Discover Celestial Phenomenon, Name It 'Steve'". 24 April 2017.
  11. ↑ "New atmospheric phenomenon named STEVE discovered by aurora watchers". ABC News. 24 April 2017.
  12. ↑ Rozell, Ned (2015-04-02). "Citizen science meets the aurora". University of Alaska Fairbanks Geophysical Institute.
  13. ↑ "7 Things to Know About "STEVE"". Aurorasaurus. 2017-03-14.
  14. ↑ Moravec, Jeff. "Meet Steve, a sky phenomenon coming into its own". StarTribune. MediaCompany. Retrieved 9 May 2019.
  15. ↑ "Meet 'Steve,' a Totally New Kind of Aurora". 2018-03-14. Archived from the original on March 15, 2018. Retrieved 2018-03-22.
  16. ↑ Saner, Emine (2018-03-19). "'Steve': the mystery purple aurora that rivals the northern lights". the Guardian. Retrieved 2018-03-22.
  17. ↑ Skywatching, Samantha Mathewson 2018-03-15T22:47:11Z (15 March 2018). "Help NASA Study 'Steve,' a Newfound Aurora Type". Space.com. Retrieved 2019-05-13.{{cite web}}: CS1 maint: numeric names: authors list (link)
  18. ↑ https://vejr.tv2.dk/2024-10-08-yderst-sjaeldent-faenomen-set-over-danmark
  19. 1 2 Garner, Rob (2018-03-14). "NASA Needs Your Help to Find Steve and Here's How". NASA. Retrieved 2018-03-22.
  20. ↑ Boisvert, Eugene. "Atmospheric phenomenon Steve spotted over south-east SA following Aurora Australis". ABC News Australia. Retrieved 17 October 2024.
  21. 1 2 MacDonald, Elizabeth A.; Donovan, Eric; Nishimura, Yukitoshi; Case, Nathan A.; Gillies, D. Megan; Gallardo-Lacourt, Bea; Archer, William E.; Spanswick, Emma L.; Bourassa, Notanee; Connors, Martin; Heavner, Matthew; Jackel, Brian; Kosar, Burcu; Knudsen, David J.; Ratzlaff, Chris; Schofield, Ian (2018-03-01). "New science in plain sight: Citizen scientists lead to the discovery of optical structure in the upper atmosphere". Science Advances. 4 (3): eaaq0030. Bibcode:2018SciA....4...30M. doi: 10.1126/sciadv.aaq0030 . ISSN   2375-2548. PMC   5851661 . PMID   29546244.
  22. ↑ Gallardo-Lacourt, B.; Liang, J.; Nishimura, Y.; Donovan, E. (20 August 2018). "On the Origin of STEVE: Particle Precipitation or Ionospheric Skyglow?". Geophysical Research Letters . 45 (16): 7968. Bibcode:2018GeoRL..45.7968G. doi: 10.1029/2018GL078509 .
  23. ↑ Kasha Patel (April 1, 2023). "How to find STEVE, the purple streak that looks like an aurora but isn't".
  24. ↑ Andrews, Robin George (3 May 2019). "Steve the odd 'aurora' revealed to be two sky shows in one". National Geographic. Archived from the original on May 4, 2019. Retrieved 4 May 2019.
  25. ↑ Nishimura, Y.; Gallardo-Lacourt, B.; Zou, Y.; Mishin, E.; Knudsen, D.J.; Donovan, E.F.; Angelopoulos, V.; Raybell, R. (16 April 2019). "Magnetospheric signatures of STEVE: Implication for the magnetospheric energy source and inter-hemispheric conjugacy". Geophysical Research Letters. 46 (11): 5637–5644. Bibcode:2019GeoRL..46.5637N. doi: 10.1029/2019GL082460 .
  26. ↑ Lipuma, Lauren. "Scientists discover what powers celestial phenomenon STEVE". AGU News. American Geophysical Union. Retrieved 4 May 2019.
  27. ↑ Dunlevie, James (2018-11-06). "Aurora Australis with bonus 'picket fence' wows southern lights chasers in Tasmania". ABC News. Australian Broadcasting Corporation. Retrieved 4 May 2019.
  28. ↑ "Aurora-chasing citizen scientists help discover a new feature of STEVE". phys.org. Retrieved 2020-11-14.
  29. ↑ "How I met Steve". Vimeo/European Space Agency. 20 March 2017.
  30. ↑ Gallardo-Lacourt, B.; Nishimura, Y.; Donovan, E.; Gillies, D.M.; Spanswick, E.; Archer, W.E.; MacDonald, E.; Knudsen, D.J. (December 2017). "On the location of Steve, the mysterious subauroral feature". AGU Fall Meeting Abstracts. 2017. Bibcode:2017AGUFMSA51B2387G.
  31. ↑ Gallardo-Lacourt, B.; Liang, J.; Nishimura, Y.; Donovan, E. (February 20, 2018). "On the Origin of STEVE: Particle Precipitation or Ionospheric Skyglow?". Geophysical Research Letters. 45 (16): 7968–7973. Bibcode:2018GeoRL..45.7968G. doi: 10.1029/2018GL078509 . S2CID   134540082.
  32. ↑ Bailey, M.; Byrne, C.; Nezic, R.; Asher, D.; Finnegan, J. (July 23, 2018). "Historical observations of STEVE". The Observatory. 138: 227–245. arXiv: 1808.01872 . Bibcode:2018Obs...138..227B.
  33. ↑ MacDonald, E.; Conde, J.M.; Kosar, B.; Lynch, K.A.; Semeter, J.L.; Zeller, N. (December 1, 2018). "What else can citizen science and 'amateur' observations reveal about STEVE?". American Geophysical Union, Fall Meeting 2018. 2018. Bibcode:2018AGUFMSM43A..09M.
  34. ↑ MacDonald, E.; Ratzlaff, C. (December 1, 2018). "From the spark to the fire, reflections on five years of public participation in aurora research". American Geophysical Union, Fall Meeting 2018. 2018. Bibcode:2018AGUFM.U51A..04M.
  35. ↑ Gallardo-Lacourt, B.; Liang, J.; Nishimura, Y.; Donovan, E.; Gillies, D.M.; Perry, G.W.; Archer, W.E.; Nava, O.; Spanswick, E.L. (December 1, 2018). "On the origin and geomagnetic conditions of STEVE's formation". American Geophysical Union, Fall Meeting 2018. 2018. Bibcode:2018AGUFMSM51E2787G.
  36. ↑ Gallardo-Lacourt, B.; Nishimura, e.; Donovan, E.; Gillies, D.M.; Perry, G.W.; Archer, W.E.; Nava, O.; Spanswick, E.L. (November 8, 2018). "A Statistical Analysis of STEVE". Journal of Geophysical Research: Space Physics. 123 (11): 9893–9905. Bibcode:2018JGRA..123.9893G. doi: 10.1029/2018JA025368 . S2CID   134931832.
  37. ↑ Gallardo-Lacourt, B.; Perry, G. W.; Archer, W. E.; Donovan, E. (March 2019). "How Did We Miss This? An Upper Atmospheric Discovery Named STEVE". Eos Science News by AGU.
  38. ↑ Gillies, D.M.; Donovan, E.; Hampton, D.; Liang, J.; Connors, M.; Nishimura, Y.; Gallardo-Lacourt, B.; Spanswick, E.L. (July 3, 2019). "First Observations From the TREx Spectrograph: The Optical Spectrum of STEVE and the Picket Fence Phenomena". Geophysical Research Letters. 46 (13): 7207–7213. Bibcode:2019GeoRL..46.7207G. doi:10.1029/2019GL083272. S2CID   198413976.
  39. ↑ Mende, S.B.; Turner, C. (June 24, 2019). "Color Ratios of Subauroral (STEVE) Arcs". Journal of Geophysical Research: Space Physics. 124 (7): 5945–5955. Bibcode:2019JGRA..124.5945M. doi:10.1029/2019JA026851. S2CID   197560558.
  40. ↑ MacDonald, E.; Hunnekuhl, M. (December 2019). "A new dataset of STEVE phenomenon related observations spanning multiple solar cycles". American Geophysical Union, Fall Meeting 2019. 2019. Bibcode:2019AGUFMSM11C3299M.
  41. ↑ Mende, S.B.; Harding, B.J.; Turner, C. (December 18, 2019). "Subauroral Green STEVE Arcs: Evidence for Low-Energy Excitation". Geophysical Research Letters. 46 (24): 14256–14262. Bibcode:2019GeoRL..4614256M. doi:10.1029/2019GL086145. S2CID   214009144.
  42. ↑ Nishimura, Y.; Gallardo-Lacourt, B.; Zou, Y.; Mishin, E.; Knudsen, D.J.; Donovan, E.; Angelopoulos, V.; Raybell, R. (April 16, 2019). "Magnetospheric Signatures of STEVE: Implications for the Magnetospheric Energy Source and Interhemispheric Conjugacy". Geophysical Research Letters. 46 (11): 5637–5644. Bibcode:2019GeoRL..46.5637N. doi: 10.1029/2019GL082460 . S2CID   146182527.
  43. ↑ Svaldi, V.C.; Matsuo, T.; Kilcommons, L.M.; MacDonald, E.; Gallardo-Lacourt, B. (December 1, 2019). "High-Latitude Ionospheric Electrodynamics Characterizing Energy and Momentum Deposition during STEVE Events Reported by Citizen Scientists". American Geophysical Union, Fall Meeting 2019. 2019. Bibcode:2019AGUFMSM11B3283S.
  44. ↑ Archer, W.E.; Gallardo-Lacourt, B.; Perry, G.W.; St.-Maurice, J.P.; Buchert, S.C.; Donovan, E. (June 4, 2019). "Steve: The Optical Signature of Intense Subauroral Ion Drifts". Geophysical Research Letters. 46 (12): 6279–6286. Bibcode:2019GeoRL..46.6279A. doi: 10.1029/2019GL082687 . S2CID   195545155.
  45. ↑ Liang, J.; Donovan, E.; Connors, M.; Gillies, D.; St-Maurice, J.P.; Jackel, B.; Gallardo-Lacourt, B.; Spanswick, E.; Chu, X. (December 3, 2019). "Optical Spectra and Emission Altitudes of Double-Layer STEVE: A Case Study". Geophysical Research Letters. 46 (23): 13630–13639. Bibcode:2019GeoRL..4613630L. doi:10.1029/2019GL085639. S2CID   212794445.
  46. ↑ Archer, W.E.; St.-Maurice, J.P.; Gallardo-Lacourt, B.; Perry, G.W.; Cully, C.M.; Donovan, E.; Gillies, G.M.; Downie, R.; Smith, J.; Eurich, D. (September 3, 2019). "The Vertical Distribution of the Optical Emissions of a Steve and Picket Fence Event". Geophysical Research Letters. 46 (19): 10719–10725. Bibcode:2019GeoRL..4610719A. doi: 10.1029/2019GL084473 . S2CID   202900390.
  47. ↑ Chu, X.; Malaspina, D.; Gallardo-Lacourt, B.; Liang, J.; Andersson, L.; Ma, Q.; Artemyev, A.; Liu, J.; Ergun, R.E.; Thaller, S.; Akbari, H.; Akbari, H.; Larsen, B.; Reeves, R.; Wygant, J.; Breneman, A.; Tian, S.; Connors, M.; Donovan, E.; Archer, W.; MacDonald, E. (November 11, 2019). "Identifying STEVE's Magnetospheric Driver Using Conjugate Observations in the Magnetosphere and on the Ground". Geophysical Research Letters. 46 (22): 12665–12674. Bibcode:2019GeoRL..4612665C. doi: 10.1029/2019GL082789 . S2CID   210258255.
  48. ↑ Mishin, E.; Streltsov, A. (December 10, 2019). "STEVE and the Picket Fence: Evidence of Feedback-Unstable Magnetosphere-Ionosphere Interaction". EPJ Web of Conferences. 46 (24): 14247–14255. Bibcode:2019GeoRL..4614247M. doi:10.1029/2019GL085446. S2CID   213702359.
  49. ↑ Erlandson, R.E. (December 1, 2019). "Possible Evidence of STEVE in Dynamics Explorer-2 Data". American Geophysical Union, Fall Meeting 2019. 2019. Bibcode:2019AGUFMSM22A..01E.
  50. ↑ Hunnekulh, M.; MacDonald, E. (February 12, 2020). "Early Ground-Based Work by Auroral Pioneer Carl Størmer on the High-Altitude Detached Subauroral Arcs Now Known as "STEVE"". Space Weather. 18 (3). Bibcode:2020SpWea..1802384H. doi: 10.1029/2019SW002384 . S2CID   213841874.
  51. ↑ Hunnekuhl, M.; MacDonald, E. (December 1, 2020). "Early Evidence of Isolated Auroral Structures in the 100 km Height Regime Observed at Subauroral Latitudes by the Aurora Pioneer Carl Størmer". American Geophysical Union, Fall Meeting 2020. 2020. Bibcode:2020AGUFMSM044..07H.
  52. ↑ Hunnekuhl, M.; MacDonald, E. (February 12, 2020). "Early Ground-Based Work by Auroral Pioneer Carl Størmer on the High-Altitude Detached Subauroral Arcs Now Known as "STEVE"". Space Weather. 18 (3). Bibcode:2020SpWea..1802384H. doi: 10.1029/2019SW002384 . S2CID   213841874.
  53. ↑ Nishimura, Y.; Yang, J.; Weygand, M.; Wang, W.; Kosar, B.; Donovan, E.; Angelopoulos, V.; Paxton, L.J.; Nishitani, N. (July 13, 2020). "Magnetospheric Conditions for STEVE and SAID: Particle Injection, Substorm Surge, and Field-Aligned Currents". Journal of Geophysical Research: Space Physics. 125 (8). Bibcode:2020JGRA..12527782N. doi:10.1029/2020JA027782. S2CID   225441915.
  54. ↑ Liang, J.; Zou, Y.; Nishimura, Y.; Donovan, E. (2021). "Neutral Wind Dynamics Preceding the STEVE Occurrence and Their Possible Preconditioning Role in STEVE Formation". Journal of Geophysical Research: Space Physics. 126 (3). Bibcode:2021JGRA..12628505L. doi:10.1029/2020JA028505. S2CID   233894542.
  55. ↑ Harding, B.J.; Mende, S.B.; Triplett, C.; Wu, Y-J.J. (March 18, 2020). "A Mechanism for the STEVE Continuum Emission". Geophysical Research Letters. 47 (7). Bibcode:2020GeoRL..4787102H. doi:10.1029/2020GL087102. S2CID   216435319.
  56. ↑ Svaldi, V.C.; Matsuo, T.; Kilcommons, L.M.; Gallardo-Lacourt, B.; McDonald, E. (December 1, 2020). "High-latitude Ionospheric Electrodynamics during STEVE Events". American Geophysical Union, Fall Meeting 2020. 2020. Bibcode:2020AGUFMSA0210010S.
  57. ↑ Nishimura, Y.; Donovan, E.; Angelopoulos, V.; Nishitani, N. (June 18, 2020). "Dynamics of Auroral Precipitation Boundaries Associated With STEVE and SAID". Journal of Geophysical Research: Space Physics. 125 (8). Bibcode:2020JGRA..12528067N. doi:10.1029/2020JA028067. S2CID   225490404.
  58. ↑ Gillies, D.M.; Liang, J.; Donovan, E.; Spanswick, E. (October 16, 2020). "The Apparent Motion of STEVE and the Picket Fence Phenomena". Geophysical Research Letters. 47 (20). Bibcode:2020GeoRL..4788980G. doi:10.1029/2020GL088980. S2CID   225138775.
  59. ↑ Dreyer, J.; Partamies, N.; Whiter, D.; Ellingsen, P.G.; Baddeley, L.; Buchert, S.C. (2021). "Characteristics of fragmented aurora-like emissions (FAEs) observed on Svalbard". Annales Geophysicae. 39 (2): 277–288. Bibcode:2021AnGeo..39..277D. doi: 10.5194/angeo-39-277-2021 . hdl: 10037/21576 . S2CID   233808838.
  60. ↑ Dreyer, J.; Partamies, N.; Whiter, D.; Ellingsen, P.G.; Baddeley, L.; Buchert, S.C. (June 30, 2020). "Fragmented Aurora-like Emissions (FAEs) as a new type of aurora-like phenomenon" (PDF). Annales Geophysicae. Archived from the original (PDF) on 11 August 2020. Retrieved 27 May 2022.
  61. ↑ Yadav, S.; Shiokawa, K.; Otsuka, Y.; Connors, M.; St Maurice, J.-P. (February 2, 2021). "Multi-Wavelength Imaging Observations of STEVE at Athabasca, Canada". Journal of Geophysical Research: Space Physics. 126 (2). Bibcode:2021JGRA..126.8622Y. doi:10.1029/2020JA028622. S2CID   234036468.
  62. ↑ Varlamov, I.; Parnikov, S.; Ievenko, I.; Baishev, D.; Shiokawa, K. (November 8, 2021). "Registration of synchronous geomagnetic pulsations and proton aurora during the substorm on March 1, 2017". EPJ Web of Conferences. 254: 02012. Bibcode:2021EPJWC.25402012V. doi: 10.1051/epjconf/202125402012 . S2CID   243901884.
  63. ↑ Martinis, C.; Nishimura, Y.; Wroten, J.; Bhatt, A.; Dyer, A.; Gallardo-Lacourt, B. (April 6, 2021). "First Simultaneous Observation of STEVE and SAR Arc Combining Data From Citizen Scientists, 630.0 nm All-Sky Images, and Satellites". Geophysical Research Letters. 48 (8). Bibcode:2021GeoRL..4892169M. doi:10.1029/2020GL092169. S2CID   233528380.
  64. ↑ Gallardo-Lacourt, B.; Frey, H.U.; Martinis, C. (January 6, 2021). "Proton Aurora and Optical Emissions in the Subauroral Region". Space Science Reviews. 217 (1): 10. Bibcode:2021SSRv..217...10G. doi:10.1007/s11214-020-00776-6. S2CID   230796229.
  65. ↑ Hunnekuhl, M.; MacDonald, E.; Swanson, B.; Voss, S.; Maynard, T.; Chernenkoff, A.; Stone, J.; Standring, W.; Stott, D.; Atkins, R.; Monk, N.; Ward, S. (December 30, 2022). "Robust techniques to improve high quality triangulations of contemporaneous citizen science observations of STEVE". AGU Poster Sessions. 2021. Bibcode:2021AGUFMSA35F1957H.
  66. ↑ Parnikov, S.G.; Ievenko, I.B.; Koltovskoy, I.I. (December 15, 2021). "Comparison of the SAR arc, STEVE and Picket fence dynamics registered at the Maimaga subauroral station on March 1, 2017". In Romanovskii, Oleg A; Matvienko, Gennadii G (eds.). 27th International Symposium on Atmospheric and Ocean Optics, Atmospheric Physics. Vol. 11916. pp. 1615–1619. Bibcode:2021SPIE11916E..7LP. doi:10.1117/12.2603112. ISBN   9781510646971. S2CID   245270235 – via SPIE Digital Library.
  67. ↑ Bennett, C.L.; Bourassa, N. (March 18, 2021). "Improved Analysis of STEVE Photographs". Journal of Geophysical Research: Space Physics. 126 (4). Bibcode:2021JGRA..12627843B. doi:10.1029/2020JA027843. S2CID   233738641.
  68. ↑ Martinis, C.; Gallardo-Lacourt, B.; Wroten, J.; Nishimura, Y.; Baumgardner, J.; Knudsen, D.J. (May 2, 2022). "Rainbow of the Night: First Direct Observation of a SAR arc evolving into STEVE". Geophysical Research Letters. 49 (11). Bibcode:2022GeoRL..4998511M. doi: 10.1029/2022GL098511 . S2CID   248703659.
  69. ↑ Lyons, L.R.; Gallardo-Lacourt, B.; Nishimura, Y. (January 1, 2022). "Auroral structures: Revealing the importance of meso-scale M-I coupling". Cross-Scale Coupling and Energy Transfer in the Magnetosphere-Ionosphere-Thermosphere System. pp. 65–101. doi:10.1016/B978-0-12-821366-7.00004-4. ISBN   9780128213667. S2CID   245030339.
  70. ↑ Gasque, L.; Janalizadeh, R.; Harding, B.; Yonker, J.; Gillies, M. (November 3, 2023). "It's Not Easy Being Green: Kinetic Modeling of the Emission Spectrum Observed in STEVE's Picket Fence". Geophysical Research Letters. 50 (21). Bibcode:2023GeoRL..5006073G. doi: 10.1029/2023GL106073 .
  71. ↑ Nishimura, Y.; Dyer, A.; Kangas, L.; Donovan, E.; Angelopoulos, V. (January 18, 2023). "Unsolved problems in Strong Thermal Emission Velocity Enhancement (STEVE) and the picket fence". Frontiers in Astronomy and Space Sciences. 50 (21): 3. Bibcode:2023FrASS..1087974N. doi: 10.3389/fspas.2023.1087974 .
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.