Tracking magnetic flux and helicity from the Sun to Earth - Multi-spacecraft analysis of a magnetic cloud and its solar source

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Volume 669 (January 2023)

A&A, 669 (2023) A72

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Solar Orbiter First Results (Nominal Mission Phase)

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Table 3.

Properties of the left-handed magnetic flux rope expelled from the solar source region (AR 12891) during an extended period of activity (a C4.5-class flare, a flare-less filament eruption, and a double-peak M-class flare) in comparison to that of the associated MC detected near Earth.

	Solar source region	Interplanetary CME/Magnetic cloud
	(low corona)	(Solar Orbiter → Earth)
Distance from Sun [AU]	0.00	0.85 → 0.98
Average magnetic field strength [G]
– Flux rope	262±126 ^(a) (200±300 ^(b))	(1.8±0.1) × 10⁻⁴ → (1.4±0.1) × 10⁻⁴
Magnetic flux [×10²¹ Mx]
– Flux rope (axial)	0.3±0.2 ^(a)	0.6±0.1 → 0.5±0.1
– Flux rope (poloidal)		0.8±0.3 → 0.7±0.3
– Flare ribbons (accumulated)	1.5±0.1
– Coronal dimmings (accumulated)	9.7±0.5
Helicity [unsigned; ×10⁴¹ Mx²]
– Flux rope	1.5±0.4	2.4±1.7 → 2.8±1.6

Notes.

^(a)

Estimated from vertical planes as exemplary shown in Figs. 3c–e, i.e., spanning ∼16 × 17 Mm².

^(b)

Back-extrapolation of in situ estimate based on the assumption of self-similarity and using the estimated power-law index derived from in situ analysis of Solar Orbiter and OMNI measurements (for details see main text).

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