Alfvén wave

An Alfvén wave is a low-frequency (compared to the ion gyrofrequency) travelling oscillation of the ions and magnetic field in a plasma. The ion mass density provides the inertia and the magnetic field line tension provides the restoring force. Alfvén waves propagate in the direction of the magnetic field, and the motion of the ions and the perturbation of the magnetic field are transverse to the direction of propagation. However, Alfvén waves existing at oblique incidences will smoothly change into magnetosonic waves when the propagation is perpendicular to the magnetic field.

Alfvén waves are dispersionless.

[[File:Alfven-wave-double-layer.gif|thumb|A cluster of double layers forming in an Alfvén wave, about a sixth of the distance from the left.

Red = electrons,

Green = ions,

Yellow = electric potential,

Orange = parallel electric field,

Pink = charge density,

Blue = magnetic field]]

The low-frequency relative permittivity $\backslash varepsilon$ of a magnetized plasma is given by{{cite book |last=Chen |first=F.F. |year=2016 |title=Introduction to Plasma Physics and Controlled Fusion |edition=3rd |publisher=Springer International Publishing |place=Switzerland |pages=55, 126–131}}

$$\backslash varepsilon\; =\; 1\; +\; \backslash frac\{c^2\backslash ,\backslash mu\_0\backslash ,\backslash rho\}\{B^2\}$$

where {{mvar|B}} is the magnetic flux density, $c$ is the speed of light, $\backslash mu\_0$ is the permeability of the vacuum, and the mass density is the sum

$$\backslash rho\; =\; \backslash sum\_s\; n\_s\; m\_s\; ,$$

over all species of charged plasma particles (electrons as well as all types of ions).

Here species $s$ has number density $n\_s$

and mass per particle $m\_s$.

The phase velocity of an electromagnetic wave in such a medium is

$$v\; =\; \backslash frac\{c\}\{\backslash sqrt\{\backslash varepsilon\}\}\; =\; \backslash frac\{c\}\{\backslash sqrt\{1\; +\; \backslash dfrac\{c^2\; \backslash mu\_0\; \backslash rho\}\{B^2\}\}\}$$

For the case of an Alfvén wave

$$v\; =\; \backslash frac\{v\_A\}\{\backslash sqrt\{1\; +\; \backslash dfrac\{v\_A^2\}\{c^2\}\}\}$$

where

$$v\_A\; \backslash equiv\; \backslash frac\{B\}\{\backslash sqrt\{\backslash mu\_0\backslash ,\backslash rho\}\}$$

is the Alfvén wave group velocity.

(The formula for the phase velocity assumes that the plasma particles are moving at non-relativistic speeds, the mass-weighted particle velocity is zero in the frame of reference, and the wave is propagating parallel to the magnetic field vector.)

If $v\_A\; \backslash ll\; c$, then $v\; \backslash approx\; v\_A$. On the other hand, when $v\_A\; \backslash to\; \backslash infty$, $v\; \backslash to\; c$. That is, at high field or low density, the group velocity of the Alfvén wave approaches the speed of light, and the Alfvén wave becomes an ordinary electromagnetic wave.

Neglecting the contribution of the electrons to the mass density, $\backslash rho\; =\; n\_i\; \backslash ,\; m\_i$, where $n\_i$ is the ion number density and $m\_i$ is the mean ion mass per particle, so that

$$v\_A\; \backslash approx\; \backslash left(2.18\; \backslash times\; 10^\{11\}\backslash ,\backslash text\{cm\}\backslash ,\backslash text\{s\}^\{-1\}\backslash right)\; \backslash left(\backslash frac\{m\_i\}\{m\_p\}\backslash right)^\{-\backslash frac\{1\}\{2\}\}\; \backslash left(\backslash frac\{n\_i\}\{1~\backslash text\{cm\}^\{-3\}\}\backslash right)^\{-\backslash frac\{1\}\{2\}\}\; \backslash left(\backslash frac\{B\}\{1~\backslash text\{G\}\}\backslash right).$$

In plasma physics, the Alfvén time $\backslash tau\_A$ is an important timescale for wave phenomena. It is related to the Alfvén velocity by:

$$\backslash tau\_A\; =\; \backslash frac\{a\}\{v\_A\}$$

where $a$ denotes the characteristic scale of the system. For example, $a$ could be the minor radius of the torus in a tokamak.

The Alfvén wave velocity in relativistic magnetohydrodynamics is{{cite journal |last=Gedalin |first=M. |year=1993 |title=Linear waves in relativistic anisotropic magnetohydrodynamics |journal=Physical Review E |volume=47 |issue=6 |pages=4354–4357 |doi=10.1103/PhysRevE.47.4354 |pmid=9960513 |bibcode=1993PhRvE..47.4354G}}

$$v\; =\; \backslash frac\{c\}\{\backslash sqrt\{1\; +\; \backslash dfrac\{e\; +\; P\}\{2\; P\_m\}\}\}$$

where {{mvar|e}} is the total energy density of plasma particles, $P$ is the total plasma pressure, and

$$P\_m\; =\; \backslash frac\{B^2\}\{2\; \backslash mu\_0\}$$

is the magnetic pressure. In the non-relativistic limit, where $P\; \backslash ll\; e\; \backslash approx\; \backslash rho\; c^2$, this formula reduces to the one given previously.

Alfvén waves can propagate in different modes depending on the plasma conditions. The most important modes include:

The classical or shear Alfvén wave is an incompressible transverse wave where the perturbations of magnetic field and velocity are perpendicular to the direction of the background magnetic field and the wave vector. In an ideal MHD plasma, these waves propagate strictly along the magnetic field lines at the Alfvén velocity.{{cite book |last=Goedbloed |first=J.P. |last2=Poedts |first2=S. |year=2004 |title=Principles of Magnetohydrodynamics: With Applications to Laboratory and Astrophysical Plasmas |publisher=Cambridge University Press |pages=226–233 |isbn=978-0-521-62347-6}}

When the perpendicular wavelength becomes comparable to the electron skin depth (c/ω_pe, where ω_pe is the electron plasma frequency) and β << m_e/m_i (where β is the ratio of plasma pressure to magnetic pressure), the wave is called an inertial Alfvén wave. In this regime, electron inertia becomes important, and the wave develops a significant parallel electric field component, making these waves important for particle acceleration in space plasmas.{{cite journal |last1=Lysak |first1=Robert L. |last2=Lotko |first2=William |title=On the kinetic dispersion relation for shear Alfvén waves |journal=Journal of Geophysical Research: Space Physics |volume=101 |issue=A3 |pages=5085–5094 |year=1996 |doi=10.1029/95JA03712 |bibcode=1996JGR...101.5085L}}

When the perpendicular wavelength becomes comparable to the ion gyroradius and β ~ 1, the wave is called a kinetic Alfvén wave. These waves arise from the coupling between shear Alfvén waves and ion acoustic waves when finite ion Larmor radius effects are included. Kinetic Alfvén waves are important for energy dissipation in space plasmas and may play a significant role in solar wind heating.{{cite journal |last1=Hasegawa |first1=Akira |last2=Chen |first2=Liu |title=Kinetic process of plasma heating due to Alfvén wave excitation |journal=Physical Review Letters |volume=35 |issue=6 |pages=370–373 |year=1975 |doi=10.1103/PhysRevLett.35.370 |bibcode=1975PhRvL..35..370H}}{{cite journal |last1=Chaston |first1=C.C. |last2=Salem |first2=C. |last3=Bonnell |first3=J.W. |last4=Carlson |first4=C.W. |last5=Ergun |first5=R.E. |last6=Strangeway |first6=R.J. |last7=McFadden |first7=J.P. |title=The Turbulent Alfvénic Aurora |journal=Physical Review Letters |volume=100 |issue=17 |pages=175003 |year=2008 |doi=10.1103/PhysRevLett.100.175003 |bibcode=2008PhRvL.100q5003C |pmid=18518340}}

The Alfvén Mach number (M_A) is a dimensionless quantity defined as the ratio of the flow velocity to the Alfvén velocity:

M_A = v/v_A

where v is the flow velocity and v_A is the Alfvén velocity. The Alfvén Mach number has several important applications:{{cite book |last=Priest |first=Eric |year=2014 |title=Magnetohydrodynamics of the Sun |publisher=Cambridge University Press |pages=181–183 |isbn=978-0-521-85471-9}}

• When M_A < 1, the flow is sub-Alfvénic, meaning that Alfvén waves can propagate upstream against the flow.
• When M_A > 1, the flow is super-Alfvénic, and Alfvén waves are swept downstream by the flow.
• At critical points where M_A = 1, important transitions in plasma behaviour occur, such as in solar wind acceleration or in magnetospheric boundary regions.

The Alfvén Mach number is particularly important in understanding the interaction of the solar wind with planetary magnetospheres, the formation of shock waves in space plasmas, and the dynamics of astrophysical jets.{{cite journal |last1=Gosling |first1=J.T. |last2=Thomsen |first2=M.F. |last3=Bame |first3=S.J. |last4=Russell |first4=C.T. |title=Accelerated plasma flows at the near-tail magnetopause |journal=Journal of Geophysical Research: Space Physics |volume=91 |issue=A3 |pages=3029–3041 |year=1986 |doi=10.1029/JA091iA03p03029 |bibcode=1986JGR....91.3029G}}{{cite journal |last1=Russell |first1=C.T. |title=The magnetopause of Earth and planets |journal=Advances in Space Research |volume=10 |issue=8 |pages=159–167 |year=1990 |doi=10.1016/0273-1177(90)90094-B |bibcode=1990AdSpR..10..159R}}

File:PIA19822-MagneticBlackHoleWaves-AlfvenS-waves-20150709.jpg jets.]]

{{Further|Stellar corona#Coronal heating problem}}

The study of Alfvén waves began from the coronal heating problem, a longstanding question in heliophysics. It was unclear why the temperature of the solar corona is hot (about one million kelvins) compared to its surface (the photosphere), which is only a few thousand kelvins. Intuitively, it would make sense to see a decrease in temperature when moving away from a heat source, but this does not seem to be the case even though the photosphere is denser and would generate more heat than the corona.

In 1942, Hannes Alfvén proposed in Nature the existence of an electromagnetic-hydrodynamic wave which would carry energy from the photosphere to heat up the corona and the solar wind. He claimed that the sun had all the necessary criteria to support these waves and they may in turn be responsible for sun spots. He stated:

If a conducting liquid is placed in a constant magnetic field, every motion of the liquid gives rise to an E.M.F. which produces electric currents. Owing to the magnetic field, these currents give mechanical forces which change the state of motion of the liquid. Thus a kind of combined electromagnetic–hydrodynamic wave is produced.{{cite journal |first=Hannes |last=Alfvén |year=1942 |title=Existence of electromagnetic–hydrodynamic waves |journal=Nature |volume=150 |issue=3805 |pages=405–406 |bibcode=1942Natur.150..405A |doi=10.1038/150405d0 |s2cid=4072220}}

This would eventually turn out to be Alfvén waves. He received the 1970 Nobel Prize in Physics for this discovery.

The convection zone of the Sun, the region beneath the photosphere in which energy is transported primarily by convection, is sensitive to the motion of the core due to the rotation of the Sun. Together with varying pressure gradients beneath the surface, electromagnetic fluctuations produced in the convection zone induce random motion on the photospheric surface and produce Alfvén waves. The waves then leave the surface, travel through the chromosphere and transition zone, and interact with the ionized plasma. The wave itself carries energy and some of the electrically charged plasma.

In the early 1990s, de Pontieu{{cite web |url=http://www.mpe.mpg.de/Highlights/FB1997/h97-10-02.html |archive-url=https://web.archive.org/web/20020716063013/http://www.mpe.mpg.de/Highlights/FB1997/h97-10-02.html |url-status=dead |archive-date=16 July 2002 |title=Chromospheric Spicules driven by Alfvén waves |author = Bart de Pontieu |publisher=Max-Planck-Institut für extraterrestrische Physik |date = 18 December 1997 |access-date=1 April 2012 }} and Haerendel{{cite journal |title=Weakly damped Alfven waves as drivers of solar chromospheric spicules |author=Gerhard Haerendel |journal=Nature |volume=360 |issue=6401 |pages=241–243 |date=1992 |bibcode=1992Natur.360..241H |doi=10.1038/360241a0 |s2cid=44454309}} suggested that Alfvén waves may also be associated with the plasma jets known as spicules. It was theorized these brief spurts of superheated gas were carried by the combined energy and momentum of their own upward velocity, as well as the oscillating transverse motion of the Alfvén waves.

In 2007, Alfvén waves were reportedly observed for the first time traveling towards the corona by Tomczyk et al., but their predictions could not conclude that the energy carried by the Alfvén waves was sufficient to heat the corona to its enormous temperatures, for the observed amplitudes of the waves were not high enough.{{cite journal |title=Alfven waves in the solar corona |author1=Tomczyk, S. |author2=McIntosh, S.W. |author3=Keil, S.L. |author4=Judge, P.G. |author5=Schad, T. |author6=Seeley, D.H. |author7=Edmondson, J. |journal=Science |volume=317 |issue=5842 |pages=1192–1196 |date=2007 |doi=10.1126/science.1143304 |pmid=17761876 |bibcode=2007Sci...317.1192T |s2cid=45840582 }} However, in 2011, McIntosh et al. reported the observation of highly energetic Alfvén waves combined with energetic spicules which could sustain heating the corona to its million-kelvin temperature. These observed amplitudes (20.0 km/s against 2007's observed 0.5 km/s) contained over one hundred times more energy than the ones observed in 2007.{{cite journal |title=Alfvenic waves with sufficient energy to power the quiet solar corona and fast solar wind. |author1=McIntosh |journal=Nature |volume=475 |issue=7357 |pages=477–480 |date=2011 |bibcode = 2011Natur.475..477M |doi=10.1038/nature10235 |display-authors=etal |pmid=21796206|s2cid=4336248}} The short period of the waves also allowed more energy transfer into the coronal atmosphere. The 50,000 km-long spicules may also play a part in accelerating the solar wind past the corona.{{cite web |url=http://www.nasa.gov/mission_pages/sdo/news/alfven-waves.html |title=SDO spots extra energy in the Sun's corona |author=Karen Fox |publisher=NASA |date=27 July 2011 |access-date=2 April 2012}} Alfvén waves are routinely observed in solar wind, in particular in fast solar wind streams. The role of Alfvénic oscillations in the interaction between fast solar wind and the Earth's magnetosphere is currently under debate.{{cite journal| last1=Pokhotelov|first1=D.| last2=Rae|first2=I.J. | last3=Murphy|first3= K.R. |last4= Mann|first4=I.R. |title= The influence of solar wind variability on magnetospheric ULF wave power| journal=Annales Geophysicae| date=2015-06-08 | volume=33|issue=6 |pages=697–701 |doi=10.5194/angeo-33-697-2015|doi-access=free|bibcode=2015AnGeo..33..697P }}{{cite journal| last1=Borovsky|first1=J.E. |title= Further investigation of the effect of upstream solar-wind fluctuations on solar-wind/magnetosphere coupling: Is the effect real?| journal= Frontiers in Astronomy and Space Sciences| date=2023-01-05 |volume=9 |page=433 |doi=10.3389/fspas.2022.975135 |doi-access=free |bibcode=2023FrASS...975135B }}

However, the above-mentioned discoveries of Alfvén waves in the complex Sun's atmosphere, starting from the Hinode era in 2007 for the next 10 years, mostly fall in the realm of Alfvénic waves essentially generated as a mixed mode due to transverse structuring of the magnetic and plasma properties in the localized flux tubes. In 2009, Jess et al. reported the periodic variation of H-alpha line-width as observed by Swedish Solar Telescope (SST) above chromospheric bright-points. They claimed first direct detection of the long-period (126–700 s), incompressible, torsional Alfvén waves in the lower solar atmosphere.

After the seminal work of Jess et al. (2009), in 2017 Srivastava et al. detected the existence of high-frequency torsional Alfvén waves in the Sun's chromospheric fine-structured flux tubes. They discovered that these high-frequency waves carry substantial energy capable of heating the Sun's corona and also originating the supersonic solar wind. In 2018, using spectral imaging observations, non-LTE (local thermodynamic equilibrium) inversions and magnetic field extrapolations of sunspot atmospheres, Grant et al. found evidence for elliptically polarized Alfvén waves forming fast-mode shocks in the outer regions of the chromospheric umbral atmosphere. They provided quantification of the degree of physical heat provided by the dissipation of such Alfvén wave modes above active region spots.

In 2024, a paper was published in the journal Science detailing a set of observations of what turned out to be the same jet of solar wind made by Parker Solar Probe and Solar Orbiter in February 2022, and implying Alfvén waves were what kept the jet's energy high enough to match the observations.{{cite journal | last1=Rivera | first1=Yeimy J. | last2=Badman | first2=Samuel T. | last3=Stevens | first3=Michael L. | last4=Verniero | first4=Jaye L. | last5=Stawarz | first5=Julia E. | last6=Shi | first6=Chen | last7=Raines | first7=Jim M. | last8=Paulson | first8=Kristoff W. | last9=Owen | first9=Christopher J. | last10=Niembro | first10=Tatiana | last11=Louarn | first11=Philippe | last12=Livi | first12=Stefano A. | last13=Lepri | first13=Susan T. | last14=Kasper | first14=Justin C. | last15=Horbury | first15=Timothy S. | last16=Halekas | first16=Jasper S. | last17=Dewey | first17=Ryan M. | last18=De Marco | first18=Rossana | last19=Bale | first19=Stuart D. | title=In situ observations of large-amplitude Alfvén waves heating and accelerating the solar wind | journal=Science | volume=385 | issue=6712 | date=August 30, 2024 | issn=0036-8075 | doi=10.1126/science.adk6953 | pages=962–966| pmid=39208109 | arxiv=2409.00267 | bibcode=2024Sci...385..962R }}

• 1942: Alfvén suggests the existence of electromagnetic-hydromagnetic waves in a paper published in [https://www.nature.com/articles/150405d0 Nature 150, 405–406 (1942).]
• 1949: Laboratory experiments by S. Lundquist produce such waves in magnetized mercury, with a velocity that approximated Alfvén's formula.
• 1949: Enrico Fermi uses Alfvén waves in his theory of cosmic rays.
• 1950: Alfvén publishes the first edition of his book, Cosmical Electrodynamics, detailing hydromagnetic waves, and discussing their application to both laboratory and space plasmas.
• 1952: Additional confirmation appears in experiments by Winston Bostick and Morton Levine with ionized helium.
• 1954: Bo Lehnert produces Alfvén waves in liquid sodium.{{Cite journal|last=Lehnert|first=Bo|date=1954-05-15|title=Magneto-Hydrodynamic Waves in Liquid Sodium|journal=Physical Review|volume=94|issue=4|pages=815–824|doi=10.1103/PhysRev.94.815|bibcode=1954PhRv...94..815L}}
• 1958: Eugene Parker suggests hydromagnetic waves in the interstellar medium.
• 1958: Berthold, Harris, and Hope detect Alfvén waves in the ionosphere after the Argus nuclear test, generated by the explosion, and traveling at speeds predicted by Alfvén formula.
• 1958: Eugene Parker suggests hydromagnetic waves in the Solar corona extending into the Solar wind.
• 1959: D. F. Jephcott produces Alfvén waves in a gas discharge.{{Cite journal|last=JEPHCOTT|first=D. F.|date=1959-06-13|title=Alfvén Waves in a Gas Discharge|journal=Nature|language=En|volume=183|issue=4676|pages=1652–1654|doi=10.1038/1831652a0|issn=0028-0836|bibcode=1959Natur.183.1652J|s2cid=11487078}}
• 1959: C. H. Kelley and J. Yenser produce Alfvén waves in the ambient atmosphere.
• 1960: Coleman et al. report the measurement of Alfvén waves by the magnetometer aboard the Pioneer and Explorer satellites.{{Cite journal|last1=Sonett|first1=C. P.|last2=Smith|first2=E. J.|last3=Judge|first3=D. L.|last4=Coleman|first4=P. J.|date=1960-02-15|title=Current Systems in the Vestigial Geomagnetic Field: Explorer VI|journal=Physical Review Letters|volume=4|issue=4|pages=161–163|doi=10.1103/PhysRevLett.4.161|bibcode=1960PhRvL...4..161S}}
• 1961: Sugiura suggests evidence of hydromagnetic waves in the Earth's magnetic field.{{Cite journal|last=Sugiura|first=Masahisa|date=Dec 1961|title=Evidence of low-frequency hydromagnetic waves in the exosphere|journal=Journal of Geophysical Research|language=en|volume=66|issue=12|pages=4087–4095|doi=10.1029/jz066i012p04087|issn=0148-0227|bibcode=1961JGR....66.4087S}}
• 1961: Normal Alfvén modes and resonances in liquid sodium are studied by [http://aero-comlab.stanford.edu/jameson/publication_list.html Jameson].
• 1966: R. O. Motz generates and observes Alfvén waves in mercury.{{Cite journal|last=Motz|first=Robin O.|date=1966|title=Alfvén Wave Generation in a Spherical System|journal=Physics of Fluids|language=en|volume=9|issue=2|pages=411–412|doi=10.1063/1.1761687|issn=0031-9171|bibcode=1966PhFl....9..411M}}
• 1970: Hannes Alfvén wins the 1970 Nobel Prize in Physics for "fundamental work and discoveries in magneto-hydrodynamics with fruitful applications in different parts of plasma physics".
• 1973: Eugene Parker suggests hydromagnetic waves in the intergalactic medium.
• 1974: J. V. Hollweg suggests the existence of hydromagnetic waves in interplanetary space.{{Cite journal|last=Hollweg|first=J. V.|date=1974|title=Hydromagnetic Waves in Interplanetary Space|journal=Publications of the Astronomical Society of the Pacific|language=en|volume=86|issue=513|pages=561|doi=10.1086/129646|issn=1538-3873|bibcode=1974PASP...86..561H|doi-access=free}}
• 1977: Mendis and Ip suggest the existence of hydromagnetic waves in the coma of Comet Kohoutek.{{Cite journal|last1=Mendis|first1=D. A.|last2=Ip|first2=W. -H.|date=Mar 1977|title=The ionospheres and plasma tails of comets|journal=Space Science Reviews|language=en|volume=20|issue=2|pages=145–190|doi=10.1007/bf02186863|issn=0038-6308|bibcode=1977SSRv...20..145M|s2cid=119883598}}
• 1984: Roberts et al. predict the presence of standing MHD waves in the solar corona{{Cite journal|last1=Roberts|first1=B.|last2=Edwin|first2=P. M.|last3=Benz|first3=A. O.|date=1984|title=Coronal oscillations|url=http://inis.iaea.org/Search/search.aspx?orig_q=RN:16011994|journal=The Astrophysical Journal|language=en|volume=279|issue=2|pages=857–865|issn=0004-637X|bibcode=1984ApJ...279..857R|doi=10.1086/161956|doi-access=free|url-access=subscription}} and opens the field of coronal seismology.
• 1999: Aschwanden et al.{{Cite journal|last1=Aschwanden|first1=Markus J.|last2=Fletcher|first2=Lyndsay|last3=Schrijver|first3=Carolus J.|last4=Alexander|first4=David|date=1999|title=Coronal Loop Oscillations Observed with the Transition Region and Coronal Explorer|journal=The Astrophysical Journal|language=en|volume=520|issue=2|pages=880|doi=10.1086/307502|issn=0004-637X|bibcode=1999ApJ...520..880A|s2cid=122698505 |url=http://eprints.gla.ac.uk/91470/1/91470.pdf}} and Nakariakov et al. report the detection of damped transverse oscillations of solar coronal loops observed with the extreme ultraviolet (EUV) imager on board the Transition Region And Coronal Explorer (TRACE), interpreted as standing kink (or "Alfvénic") oscillations of the loops. This confirms the theoretical prediction of Roberts et al. (1984).
• 2007: Tomczyk et al. reported the detection of Alfvénic waves in images of the solar corona with the Coronal Multi-Channel Polarimeter (CoMP) instrument at the National Solar Observatory, New Mexico.{{Cite journal|last1=Tomczyk|first1=S.|last2=McIntosh|first2=S. W.|last3=Keil|first3=S. L.|last4=Judge|first4=P. G.|last5=Schad|first5=T.|last6=Seeley|first6=D. H.|last7=Edmondson|first7=J.|date=2007-08-31|title=Alfvén Waves in the Solar Corona|journal=Science|language=en|volume=317|issue=5842|pages=1192–1196|doi=10.1126/science.1143304|issn=0036-8075|pmid=17761876|bibcode=2007Sci...317.1192T|s2cid=45840582}} However, these observations turned out to be kink waves of coronal plasma structures.{{Cite journal|last1=Doorsselaere|first1=T. Van|last2=Nakariakov|first2=V. M.|last3=Verwichte|first3=E.|date=2008|title=Detection of Waves in the Solar Corona: Kink or Alfvén?|journal=The Astrophysical Journal Letters|language=en|volume=676|issue=1|pages=L73|doi=10.1086/587029|issn=1538-4357|bibcode=2008ApJ...676L..73V|doi-access=free}}doi:10.1051/0004-6361/200911840
• 2007: A special issue on the Hinode space observatory was released in the journal Science.{{Cite journal|date=2007-12-07|title=Science: 318 (5856)|url=https://www.science.org/toc/science/318/5856|journal=Science|language=en|volume=318|issue=5856|issn=0036-8075}} Alfvén wave signatures in the coronal atmosphere were observed by Cirtain et al.,{{Cite journal|last1=Cirtain|first1=J. W.|last2=Golub|first2=L.|last3=Lundquist|first3=L.|last4=Ballegooijen|first4=A. van|last5=Savcheva|first5=A.|last6=Shimojo|first6=M.|last7=DeLuca|first7=E.|last8=Tsuneta|first8=S.|last9=Sakao|first9=T.|date=2007-12-07|title=Evidence for Alfvén Waves in Solar X-ray Jets|journal=Science|language=en|volume=318|issue=5856|pages=1580–1582|doi=10.1126/science.1147050|issn=0036-8075|pmid=18063786|bibcode=2007Sci...318.1580C|s2cid=39318753}} Okamoto et al.,{{Cite journal|last1=Okamoto|first1=T. J.|last2=Tsuneta|first2=S.|last3=Berger|first3=T. E.|last4=Ichimoto|first4=K.|last5=Katsukawa|first5=Y.|last6=Lites|first6=B. W.|last7=Nagata|first7=S.|last8=Shibata|first8=K.|last9=Shimizu|first9=T.|date=2007-12-07|title=Coronal Transverse Magnetohydrodynamic Waves in a Solar Prominence|journal=Science|language=en|volume=318|issue=5856|pages=1577–1580|doi=10.1126/science.1145447|issn=0036-8075|pmid=18063785|arxiv=0801.1958|bibcode=2007Sci...318.1577O|s2cid=121422620}} and De Pontieu et al.{{Cite journal|last1=Pontieu|first1=B. De|last2=McIntosh|first2=S. W.|last3=Carlsson|first3=M.|last4=Hansteen|first4=V. H.|last5=Tarbell|first5=T. D.|last6=Schrijver|first6=C. J.|last7=Title|first7=A. M.|last8=Shine|first8=R. A.|last9=Tsuneta|first9=S.|date=2007-12-07|title=Chromospheric Alfvénic Waves Strong Enough to Power the Solar Wind|journal=Science|language=en|volume=318|issue=5856|pages=1574–1577|doi=10.1126/science.1151747|issn=0036-8075|pmid=18063784|bibcode=2007Sci...318.1574D|s2cid=33655095}} By estimating the observed waves' energy density, De Pontieu et al. have shown that the energy associated with the waves is sufficient to heat the corona and accelerate the solar wind.
• 2008: Kaghashvili et al. uses driven wave fluctuations as a diagnostic tool to detect Alfvén waves in the solar corona.{{cite journal | bibcode = 2009ApJ...703.1318K | title=Driven Waves as a Diagnostics Tool in the Solar Corona | journal=The Astrophysical Journal | volume=703 | issue=2 | page=1318 | year=2009 |author1=Kaghashvili, Edisher Kh. |author2=Quinn, Richard A. |author3=Hollweg, Joseph V. | doi=10.1088/0004-637x/703/2/1318| s2cid=120848530 | doi-access=free }}
• 2009: Jess et al. detect torsional Alfvén waves in the structured Sun's chromosphere using the Swedish Solar Telescope.{{Cite journal|last1=Jess|first1=David B.|last2=Mathioudakis|first2=Mihalis|last3=Erdélyi|first3=Robert|last4=Crockett|first4=Philip J.|last5=Keenan|first5=Francis P.|last6=Christian|first6=Damian J.|date=2009-03-20|title=Alfvén Waves in the Lower Solar Atmosphere|journal=Science|language=en|volume=323|issue=5921|pages=1582–1585|doi=10.1126/science.1168680|issn=0036-8075|pmid=19299614|arxiv=0903.3546|bibcode=2009Sci...323.1582J|hdl=10211.3/172550|s2cid=14522616}}
• 2011: Alfvén waves are shown to propagate in a liquid metal alloy made of Gallium.{{cite journal |title=Experimental evidence of Alfvén wave propagation in a Gallium alloy |author=Thierry Alboussière |author2=Philippe Cardin |author3=François Debray|author4=Patrick La Rizza |author5=Jean-Paul Masson|author6=Franck Plunian |author7=Adolfo Ribeiro|author8=Denys Schmitt |journal=Phys. Fluids |volume=23 |issue=9 |page=096601 |date=2011 |doi=10.1063/1.3633090|bibcode = 2011PhFl...23i6601A |arxiv = 1106.4727 |s2cid=2234120 }}
• 2017: 3D numerical modelling performed by Srivastava et al. show that the high-frequency (12–42 mHz) Alfvén waves detected by the Swedish Solar Telescope can carry substantial energy to heat the Sun's inner corona.{{Cite journal|last1=Srivastava|first1=Abhishek Kumar|last2=Shetye|first2=Juie|last3=Murawski|first3=Krzysztof|last4=Doyle|first4=John Gerard|last5=Stangalini|first5=Marco|last6=Scullion|first6=Eamon|last7=Ray|first7=Tom|last8=Wójcik|first8=Dariusz Patryk|last9=Dwivedi|first9=Bhola N.|date=2017-03-03|title=High-frequency torsional Alfvén waves as an energy source for coronal heating|journal=Scientific Reports|language=En|volume=7|issue=1|pages=43147|doi=10.1038/srep43147|pmid=28256538|pmc=5335648|issn=2045-2322|bibcode=2017NatSR...743147S}}
• 2018: Using spectral imaging observations, non-LTE inversions and magnetic field extrapolations of sunspot atmospheres, Grant et al. found evidence for elliptically polarized Alfvén waves forming fast-mode shocks in the outer regions of the chromospheric umbral atmosphere. For the first time, these authors provided quantification of the degree of physical heat provided by the dissipation of such Alfvén wave modes.{{Citation |last1=Grant |first1=Samuel D. T. |last2=Jess |first2=David B. |last3=Zaqarashvili |first3=Teimuraz V. |last4=Beck |first4=Christian |last5=Socas-Navarro |first5=Hector |last6=Aschwanden |first6=Markus J. |last7=Keys |first7=Peter H. |last8=Christian |first8=Damian J. |last9=Houston |first9=Scott J. |last10=Hewitt |first10=Rebecca L. |title=Alfvén Wave Dissipation in the Solar Chromosphere |journal=Nature Physics |volume=14 |issue=5 |pages=480–483 |date=2018 |doi= 10.1038/s41567-018-0058-3|bibcode=2018NatPh..14..480G |arxiv=1810.07712 |s2cid=119089600 }}
• 2024: Alfvén waves are implied to be behind a smaller than expected energy loss in solar wind jets out as far as Venus' orbit, based on Parker Solar Probe and Solar Orbiter observations only two days apart.

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• Alfvén surface
• Computational magnetohydrodynamics
• Electrohydrodynamics
• Electromagnetic pump
• Ferrofluid
• Magnetic flow meter
• Magnetohydrodynamic turbulence
• MHD generator
• MHD sensor
• Molten salt
• Plasma stability
• Shocks and discontinuities (magnetohydrodynamics)

{{div col end}}

{{Reflist}}

• {{Citation |last=Alfvén |first=H. |title=Cosmic Plasma |location=Holland |publisher=Reidel |date=1981 |isbn=978-90-277-1151-9 }} — Comprehensive text by Hannes Alfvén himself, providing in-depth coverage of plasma physics including Alfvén waves.
• {{Citation |last1=Jess |first1=David B. |last2=Mathioudakis |first2=Mihalis |last3=Erdélyi |first3=Robert |last4=Crockett |first4=Philip J. |last5=Keenan |first5=Francis P. |last6=Christian |first6= Damian J. |title=Alfvén Waves in the Lower Solar Atmosphere |journal=Science |volume=323 |issue=5921 |pages=1582–1585 |date=2009 |doi=10.1126/science.1168680 |pmid=19299614 |bibcode=2009Sci...323.1582J|arxiv=0903.3546 |hdl=10211.3/172550 |s2cid=14522616 }} — First detection of torsional Alfvén waves in the structured chromosphere of the Sun.
• {{Citation |last1=Srivastava |first1=Abhishek K. |last2=Shetye |first2=Juie |last3=Murawski |first3=Krzysztof |last4=Doyle |first4=John Gerard |last5=Stangalini |first5=Marco |last6=Scullion |first6=Eamon |last7=Ray |first7=Tom |last8=Wójcik |first8=Dariusz Patryk |last9=Dwivedi |first9=Bhola N. |title=High-frequency torsional Alfvén waves as an energy source for coronal heating |journal=Scientific Reports |volume=7 |pages=id.43147 |date=2017 |doi=10.1038/srep43147 |pmid=28256538 |pmc=5335648 |bibcode=2017NatSR...743147S}} — Research demonstrating how high-frequency torsional Alfvén waves may provide energy for solar coronal heating.
• {{Citation |last1=Tomczyk |first1=S. |last2=McIntosh |first2=S. W. |last3=Keil |first3=S. L. |last4=Judge |first4=P. G. |last5=Schad |first5=T. |last6=Seeley |first6=D. H. |last7=Edmondson |first7=J. |title=Waves in the Solar Corona |journal=Science |volume=317 |issue=5842 |pages=1192–1196 |date=2007 |doi=10.1126/science.1143304 |pmid=17761876 |bibcode=2007Sci...317.1192T |s2cid=45840582 }} — Groundbreaking observational study that reported detection of Alfvénic waves in the solar corona.

• [http://www.space.com/scienceastronomy/070830_sun_waves.html Mysterious Solar Ripples Detected] Dave Mosher 2 September 2007 Space.com
• [http://www.eurekalert.org/pub_releases/2007-12/aaft-hmd113007.php EurekAlert! notification of 7 December 2007 Science special issue]
• [http://www.eurekalert.org/pub_releases/2009-03/uos-sfs032009.php EurekAlert! notification: "Scientists find solution to solar puzzle"]

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Category:Waves in plasmas