A method for determining corotating interaction regions in the equatorial plane of the heliosphere from solar wind velocity data

Abstract

Geoph•,Mcal In.sl/lule. Un/vc/'•s/lv o/ ,qlas/,a An Euler-Laorange coordinate transtbrmation •.s applied to a compt•ted solar wind velocity data ,,et lo obtain fluid streamlines which are also magnetic field lines. Plolting these lines high-resolul•on simulation data provides delailed intbrmal•on aboul the time variation of torotatung interaction regions in the equalorial plane of the hellosphere. 13,692 Olmsted and Akasofu: Brief Reporl O!msted anti Akasofu' Brief Reporl 13,693 /tcl, nowledgmems The work reporled herc was supported •n particle stream flow willa application to solar wind par! by a gran! from the National Aeronautics and Space simulation, Planet. Space Sci. 33, 831, 1985. Administration (NSG 7447) and the National Science Foundation Pizzo, V. J., A three-dfmensional model of corotating streams in (ATM 85-114512). The Editor thanks R. S Steinolt•son and B T Thomas their assistance in evaluating this paper. REFERENCES &kasot•, ,q ! • Fill•us. W Sun, C. Fry, and M. Dryer. ,• ,,•l•l;.il•O• xlt•tJ\ ot lwo nla.jor events in the heliosi•hcrc dtlt•ne the presen! •t•nspot cycle, J Geop?.s. Res., 90, 8193, the solar wind, 1, Theoretical tbundation, J Geohv.s Re•s. 83. 5563, 1978. P•z>,o, V J., A three-dimensional model of cotorating streams the solar wind, 2, Hydrod)namic •treams. J Geophvx Re.s, Pi//o, V J., A three-dimensional model of cotorating streams the solar •i•ti, 3, Magnetoh)cirodvnamic streams, J Res 87, 4374, 1982. Smith. Z. k. M. Dryer and R. S. Steinolfson, A slt•clx oJ' the tbrmation. c•olulion and ctecax of shocks •} lhc heliosphone between 0.5 and 30.0 AU, J. Gcoi)hvs Res. 90. 217, 1985.AitVen H The .sun'.,, ecneral magnetic field, 7k, lht.s. 8. 1, 1956 Sleinolf.,,on, R. S., M. Dryer and 5. Nakagawa, Numerical Burlaga L F. F B.•McDonalci, N. F. Ness, R. Schwenn, A MHD •imulation of interplanetarx shock pairs, J. Geophvs J La/a•u•. and F Mariani, Interplanetar• tlo• •xslcms Re• 80. 1223, 1975. associated with cosmic rav modulation in 1977-19•0, J •Vhano 5' C. A magnelohvdrodvnamic model tbr corotating Ge(,!)ln's R•,s 80, h579, 198•.

Near real‐time predictions of the arrival at Earth of flare‐related shocks during Solar Cycle 23

“…However, internal algorithms adjust fluid parcel positions to account for fast‐stream/slow‐stream interactions, compression of the plasma, and evolution of the interplanetary magnetic field (IMF). For details, see Hakamada and Akasofu [1982], Olmsted and Akasofu [1986], and Fry and Akasofu [1987].…”

“…The predicted SATs are extracted from automatic scans of the temporal profiles of the dynamic pressure simulated at L1 using a shock search index (SSI H ): where P is either the dynamic pressure or momentum flux; ΔP is the difference in P during consecutive 1‐hour time steps, and P min is the minimum P value for these time steps. The HAFv.2 model was originally calibrated using 1‐D models [ Sun et al , 1985; Olmsted and Akasofu , 1986; Fry and Akasofu , 1987]. More recently, Fry et al [2003] used 173 events recorded (see above) during the rise phase of Solar Cycle 23, to set the threshold now routinely used by HAFv.2 to identify shock arrivals.…”

Vortex Generation and Auroral Response to a Solar Wind Dynamic Pressure Increase: Event Analyses

“…Positive solar wind dynamic pressure (SW P dyn ) pulse events, some originate from various solar wind structures, including the leading edge of HPS (Heliospheric Plasma Sheet; e.g., Shi, Hartinger, et al., 2013; Winterhalter et al., 1994), CIR (Corotating Interaction Region; e.g., Olmsted & Akasofu, 1986) or Coronal Mass Ejection (CME; e.g., Marcia & Raymond, 1997). These can cause the compression of Earth's magnetosphere after their arrival (e.g., Li et al., 2011, 2017, 2008; Shi, Zong, et al., 2013, 2014, 2020, 2009; Russell et al., 2000, 1999; Wilken et al., 1982; Zong et al., 2004).…”

Space Weather

“…(cf. Farrugia et al, 1995;Marubashi, 1997;Gonzalez et al, 1998Luhmann, 1998, Lu et al, 1998;Osherovich et al, 1999;Rust, 1999;. Perhaps some efforts are needed to standardize such terms.…”

“…Thus, by integrat ing the velocity as a function of time graphically, one can determine the distance traveled by individual particles. This method has been carefully calibrated on the basis of MHD solutions by Olmsted and Akasofu (1985), , and Olmsted and Akasofu (1986).…”