Scale and Time Dependence of Alfvénicity in the Solar Wind as Observed by the Parker Solar Probe

Alfvénicity is a well-known property, common in the solar wind, characterized by a high correlation between magnetic and velocity fluctuations. Data from the Parker Solar Probe (PSP) enable the study of this property closer to the Sun than ever before, as well as in the sub-Alfvénic solar wind. We c...
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Autor*in:	Panisara Thepthong [verfasserIn] Peera Pongkitiwanichakul [verfasserIn] David Ruffolo [verfasserIn] Rungployphan Kieokaew [verfasserIn] Riddhi Bandyopadhyay [verfasserIn] William H. Matthaeus [verfasserIn] Tulasi N. Parashar [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2024

Schlagwörter:	Alfvén waves Interplanetary magnetic fields Interplanetary turbulence Solar wind

Übergeordnetes Werk:	In: The Astrophysical Journal - IOP Publishing, 2022, 962(2024), 1, p 37
Übergeordnetes Werk:	volume:962 ; year:2024 ; number:1, p 37

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-4357/ad1592

Katalog-ID:	DOAJ094867410

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allfields	10.3847/1538-4357/ad1592 doi (DE-627)DOAJ094867410 (DE-599)DOAJed0b1d63dae84101ae69c4c496ca8f74 DE-627 ger DE-627 rakwb eng QB460-466 Panisara Thepthong verfasserin aut Scale and Time Dependence of Alfvénicity in the Solar Wind as Observed by the Parker Solar Probe 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Alfvénicity is a well-known property, common in the solar wind, characterized by a high correlation between magnetic and velocity fluctuations. Data from the Parker Solar Probe (PSP) enable the study of this property closer to the Sun than ever before, as well as in the sub-Alfvénic solar wind. We consider scale-dependent measures of Alfvénicity based on second-order functions of the magnetic and velocity increments as a function of time lag, including the normalized cross helicity σ _c and residual energy σ _r . Scale-dependent Alfvénicity is strongest for lags near the correlation scale and increases when moving closer to the Sun. We find that σ _r typically remains close to the maximally negative value compatible with σ _c . We did not observe significant changes in measures of Alfvénicity between sub-Alfvénic and super-Alfvénic wind. During most times, the solar wind was highly Alfvénic; however, lower Alfvénicity was observed when PSP approached the heliospheric current sheet or other magnetic structures with sudden changes in the radial magnetic field, non-unidirectional strahl electron pitch angle distributions, and strong electron density contrasts. These results are consistent with a picture in which Alfvénic fluctuations generated near the photosphere transport outward, forming highly Alfvénic states in the young solar wind, and subsequent interactions with large-scale structures and gradients lead to weaker Alfvénicity, as commonly observed at larger heliocentric distances. Alfvén waves Interplanetary magnetic fields Interplanetary turbulence Solar wind Astrophysics Peera Pongkitiwanichakul verfasserin aut David Ruffolo verfasserin aut Rungployphan Kieokaew verfasserin aut Riddhi Bandyopadhyay verfasserin aut William H. Matthaeus verfasserin aut Tulasi N. Parashar verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 962(2024), 1, p 37 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:962 year:2024 number:1, p 37 https://doi.org/10.3847/1538-4357/ad1592 kostenfrei https://doaj.org/article/ed0b1d63dae84101ae69c4c496ca8f74 kostenfrei https://doi.org/10.3847/1538-4357/ad1592 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 962 2024 1, p 37
spelling	10.3847/1538-4357/ad1592 doi (DE-627)DOAJ094867410 (DE-599)DOAJed0b1d63dae84101ae69c4c496ca8f74 DE-627 ger DE-627 rakwb eng QB460-466 Panisara Thepthong verfasserin aut Scale and Time Dependence of Alfvénicity in the Solar Wind as Observed by the Parker Solar Probe 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Alfvénicity is a well-known property, common in the solar wind, characterized by a high correlation between magnetic and velocity fluctuations. Data from the Parker Solar Probe (PSP) enable the study of this property closer to the Sun than ever before, as well as in the sub-Alfvénic solar wind. We consider scale-dependent measures of Alfvénicity based on second-order functions of the magnetic and velocity increments as a function of time lag, including the normalized cross helicity σ _c and residual energy σ _r . Scale-dependent Alfvénicity is strongest for lags near the correlation scale and increases when moving closer to the Sun. We find that σ _r typically remains close to the maximally negative value compatible with σ _c . We did not observe significant changes in measures of Alfvénicity between sub-Alfvénic and super-Alfvénic wind. During most times, the solar wind was highly Alfvénic; however, lower Alfvénicity was observed when PSP approached the heliospheric current sheet or other magnetic structures with sudden changes in the radial magnetic field, non-unidirectional strahl electron pitch angle distributions, and strong electron density contrasts. These results are consistent with a picture in which Alfvénic fluctuations generated near the photosphere transport outward, forming highly Alfvénic states in the young solar wind, and subsequent interactions with large-scale structures and gradients lead to weaker Alfvénicity, as commonly observed at larger heliocentric distances. Alfvén waves Interplanetary magnetic fields Interplanetary turbulence Solar wind Astrophysics Peera Pongkitiwanichakul verfasserin aut David Ruffolo verfasserin aut Rungployphan Kieokaew verfasserin aut Riddhi Bandyopadhyay verfasserin aut William H. Matthaeus verfasserin aut Tulasi N. Parashar verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 962(2024), 1, p 37 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:962 year:2024 number:1, p 37 https://doi.org/10.3847/1538-4357/ad1592 kostenfrei https://doaj.org/article/ed0b1d63dae84101ae69c4c496ca8f74 kostenfrei https://doi.org/10.3847/1538-4357/ad1592 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 962 2024 1, p 37
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author	Panisara Thepthong
spellingShingle	Panisara Thepthong misc QB460-466 misc Alfvén waves misc Interplanetary magnetic fields misc Interplanetary turbulence misc Solar wind misc Astrophysics Scale and Time Dependence of Alfvénicity in the Solar Wind as Observed by the Parker Solar Probe
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topic_title	QB460-466 Scale and Time Dependence of Alfvénicity in the Solar Wind as Observed by the Parker Solar Probe Alfvén waves Interplanetary magnetic fields Interplanetary turbulence Solar wind
topic	misc QB460-466 misc Alfvén waves misc Interplanetary magnetic fields misc Interplanetary turbulence misc Solar wind misc Astrophysics
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title	Scale and Time Dependence of Alfvénicity in the Solar Wind as Observed by the Parker Solar Probe
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title_full	Scale and Time Dependence of Alfvénicity in the Solar Wind as Observed by the Parker Solar Probe
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title_sort	scale and time dependence of alfvénicity in the solar wind as observed by the parker solar probe
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title_auth	Scale and Time Dependence of Alfvénicity in the Solar Wind as Observed by the Parker Solar Probe
abstract	Alfvénicity is a well-known property, common in the solar wind, characterized by a high correlation between magnetic and velocity fluctuations. Data from the Parker Solar Probe (PSP) enable the study of this property closer to the Sun than ever before, as well as in the sub-Alfvénic solar wind. We consider scale-dependent measures of Alfvénicity based on second-order functions of the magnetic and velocity increments as a function of time lag, including the normalized cross helicity σ _c and residual energy σ _r . Scale-dependent Alfvénicity is strongest for lags near the correlation scale and increases when moving closer to the Sun. We find that σ _r typically remains close to the maximally negative value compatible with σ _c . We did not observe significant changes in measures of Alfvénicity between sub-Alfvénic and super-Alfvénic wind. During most times, the solar wind was highly Alfvénic; however, lower Alfvénicity was observed when PSP approached the heliospheric current sheet or other magnetic structures with sudden changes in the radial magnetic field, non-unidirectional strahl electron pitch angle distributions, and strong electron density contrasts. These results are consistent with a picture in which Alfvénic fluctuations generated near the photosphere transport outward, forming highly Alfvénic states in the young solar wind, and subsequent interactions with large-scale structures and gradients lead to weaker Alfvénicity, as commonly observed at larger heliocentric distances.
abstractGer	Alfvénicity is a well-known property, common in the solar wind, characterized by a high correlation between magnetic and velocity fluctuations. Data from the Parker Solar Probe (PSP) enable the study of this property closer to the Sun than ever before, as well as in the sub-Alfvénic solar wind. We consider scale-dependent measures of Alfvénicity based on second-order functions of the magnetic and velocity increments as a function of time lag, including the normalized cross helicity σ _c and residual energy σ _r . Scale-dependent Alfvénicity is strongest for lags near the correlation scale and increases when moving closer to the Sun. We find that σ _r typically remains close to the maximally negative value compatible with σ _c . We did not observe significant changes in measures of Alfvénicity between sub-Alfvénic and super-Alfvénic wind. During most times, the solar wind was highly Alfvénic; however, lower Alfvénicity was observed when PSP approached the heliospheric current sheet or other magnetic structures with sudden changes in the radial magnetic field, non-unidirectional strahl electron pitch angle distributions, and strong electron density contrasts. These results are consistent with a picture in which Alfvénic fluctuations generated near the photosphere transport outward, forming highly Alfvénic states in the young solar wind, and subsequent interactions with large-scale structures and gradients lead to weaker Alfvénicity, as commonly observed at larger heliocentric distances.
abstract_unstemmed	Alfvénicity is a well-known property, common in the solar wind, characterized by a high correlation between magnetic and velocity fluctuations. Data from the Parker Solar Probe (PSP) enable the study of this property closer to the Sun than ever before, as well as in the sub-Alfvénic solar wind. We consider scale-dependent measures of Alfvénicity based on second-order functions of the magnetic and velocity increments as a function of time lag, including the normalized cross helicity σ _c and residual energy σ _r . Scale-dependent Alfvénicity is strongest for lags near the correlation scale and increases when moving closer to the Sun. We find that σ _r typically remains close to the maximally negative value compatible with σ _c . We did not observe significant changes in measures of Alfvénicity between sub-Alfvénic and super-Alfvénic wind. During most times, the solar wind was highly Alfvénic; however, lower Alfvénicity was observed when PSP approached the heliospheric current sheet or other magnetic structures with sudden changes in the radial magnetic field, non-unidirectional strahl electron pitch angle distributions, and strong electron density contrasts. These results are consistent with a picture in which Alfvénic fluctuations generated near the photosphere transport outward, forming highly Alfvénic states in the young solar wind, and subsequent interactions with large-scale structures and gradients lead to weaker Alfvénicity, as commonly observed at larger heliocentric distances.
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title_short	Scale and Time Dependence of Alfvénicity in the Solar Wind as Observed by the Parker Solar Probe
url	https://doi.org/10.3847/1538-4357/ad1592 https://doaj.org/article/ed0b1d63dae84101ae69c4c496ca8f74 https://doaj.org/toc/1538-4357
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Scale and Time Dependence of Alfvénicity in the Solar Wind as Observed by the Parker Solar Probe

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