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An Empirical 3D Model of the Large-Scale Coronal Structure Astronomy & Astrophysics manuscript no. ms4 c ESO 2018 April 11, 2018 An Empirical 3D Model of the Large-scale Coronal Structure Based on the Distribution of Prominences on the Solar Disk Huw Morgan and S. Rifai Habbal Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA e-mail: [email protected] Recieved September 25, 2006 ABSTRACT Context. Despite the wealth of solar data currently available, the explicit connection between coronal streamers and features on the solar disk remains unresolved. Aims. An empirical three-dimensional model, which reproduces the evolution of the large-scale coronal structure starting from the solar surface, is presented. The model is based on the view that the source of the large-scale coronal structure, namely streamers, is a consequence of the evolution of twisted sheet-like structures originating from prominences (or, equivalently, filaments) at the base of the corona. Methods. A 3D model is created whereby high-density sheets are placed above prominences on the solar disk, which evolve and merge with height into a final radial configuration constrained by the oberved position of streamers stalks higher up in the corona. The observational constraints are provided by white light observations from the LASCO/C2 data during the declining phase of solar activity, spanning the end of Carrington Rotation (CR) 2005 and the start of CR 2006, i.e. July-August 2003, and the position of filaments from the corresponding Hα synoptic maps of the Paris-Meudon Observatory. Results. The 3D model thus derived yields a reasonable agreement with the observed large-scale coronal structure, in particular the shape of large helmet streamers. Conclusions. These results give confidence in the underlying assumption that large helmet streamers can be the result of the conver- gence of two or more sheet-like structures originating from a distribution of prominences on the solar disk. The model supports the view that streamers, during that time of the solar cycle, are often associated with multiple current sheets. Key words. sun – corona – prominences 1. INTRODUCTION sity across the streamer sheet. All these empirical models give a valuable measurement of density, and the 3D distribution of Establishing connections between observed features in the density in the corona, but cannot, or are not directly aimed at, chromosphere or low in the corona, and structures higher in resolving the link between structures in the corona and features the corona, is challenging to achieve directly from observa- on the solar disk. tions due to the complexity of the corona at low heights. Streamers are structures in the corona with densities around arXiv:astro-ph/0610219v1 6 Oct 2006 Recent improvements in observations, particularly using space- 3 to 10 times higher than surrounding regions (Schmidt 1953; craft coronagraphs such as the High Altitude Observatory’s Woo& Habbal 1999, for example). They are large and of- white-light coronagraph aboard Skylab, SPARTAN, or the ten long-lived structures which extend from the base of the Solar and Heliospheric Observatory (SOHO) Large Angle and corona out into the interplanetary solar wind (Li et al. 2002). Spectrometric Coronagraph Experiment (LASCO) C2 instru- Their sources on the solar surface are areas of enhanced ment (Brueckner et al. 1995), have allowed sophisticated anal- magnetic activity - active regions associated with sunspots or yses of coronal structure. Guhathakurta et al. (1996) created a prominences (Loucif & Koutchmy 1989; Koutchmy & Livshits 3D model of coronal density in relation to the equatorial current 1992). Prominences (or filaments when viewed against the so- sheet during solar minimum. This model was further developed lar disk) are cool, high-density ribbons of material which lie by Gibson et al. (2003) to include more complex structures, in in the hot and tenuous corona. The association of large hel- particular streamers at mid-latitude. Uninterrupted observations met streamers with prominences in the low solar atmosphere of the solar corona over the course of half a rotation or longer has, for many decades, been made from eclipse observations has made solar rotational tomography possible (Davila 1994; (see Saito & Tandberg-Hanssen (1973), and references within). Zidowitz 1999; Frazin 2000, for example). These tomographic Bˇel´ık et al. (2004) have shown, from a whole solar cycle anal- reconstructions have concentrated on the solar minimum corona. ysis of the white light and the 530.3 nm emission corona, that A detailed 3D reconstruction of density within a streamer sheet the distribution of helmet streamers migrates with the distribu- at heights above 2.5R⊙ is made by Thernisien & Howard (2006), tion of prominences. Perhaps contradictory, Liewer et al. (2001) where the face- and edge-on appearance of an isolated high- studied 8 major streamers during April 1998, and found a strong latitude streamer with solar rotation is used to constrain both the correlation between their alignment and the position of active electron density as a function of height, and the variation of den- regions on the disk. In this work, we build an empirical 3D model of the large- Send offprint requests to: Huw Morgan scale structure of the corona. The model is based on the as- 2 Morgan & Habbal: Empirical Model of Coronal Structure Based on Prominences sumption that high-densitysheets arise from filaments (or promi- nences) in the chromosphere.Constraints on the position of these sheets are imposed by disk observations of Hα filaments. These sheets are forced, with increasing height, to twist and merge, and form the stalks of streamers as observed by the LASCO C2 coronagraph at heights above where the corona becomes radial (or very close to radial), providing a constraint on their position in the extended corona.The agreement between the modeled and observed coronal images, and the simulation of the changing ap- pearance of the corona with solar rotation, is then a test of the basic assumptions used to build the model. Observations showing the large-scale coronal structure dur- ing the end of CR 2005, and the start of CR 2006 are shown in section 2. The density model is described in section 3 and the images calculated from the model are compared to observations in section 4. The merits of the model in exploring structure, sug- gestions for improvements, and the implications of the results are discussed in section 5. Conclusions are given in section 6. 2. Observations Figure 1A shows the structure of the corona on 2003/08/08 19:00. The image is composed of the SOHO Extreme Ultraviolet Fig. 1. Composite images of the corona made during (A) 1 Imaging Telescope (EIT) observations of the Extreme August 2003, (B) 18 January 1997 (solar minimum), and (C) UltraViolet (EUV) Fe IX/X 171Å lines (Delaboudiniere et al. 8 December 2000 (solar maximum). The innermost views of the 1995), and polarized brightness (pB) observations by the Mauna disk and low corona are EIT images of the Fe IX/X 171Å line, Loa Solar Observatory’s (MLSO) MK IV coronameter and except for the solar minimum disk which shows the He II 304Å the LASCO C2 coronagraph (see Fisheret al. (1981) for a line. The corona from 1.15 to 2.3 R are from the MLSO coro- description of the MLSO MKIII coronameter). At heights ⊙ nameters and above 2.3 R from the LASCO C2 coronagraph. above the limb, the images have been processed using a ⊙ (D) Detail of the large north-west helmet streamer seen in A. Normalizing Radial-Graded Filter (NRGF), described by The position of prominences and an active region at the limb are Morgan et al. (2006). The NRGF calculates the average and shown as crosses. standard deviation of brightness as a function of height within an image, and uses these values to normalize the brightness at each height. Therefore viewing the coronal structure seen near longitude 10-30◦, seen in the disk synoptic map of Fig. 3A. in a NRGF-processed image is equivalent to viewing a large The most prominent structures in Fig. 2, however, are the two set of normalized latitudinal profiles simultaneously. Images of streamers highlighted by dashed and dot-dashed lines at the west the corona made near the minimum and maximum of activity and east limb respectively. These drift slowly in latitude and do shown in Figs. 1B and 1C show that the general large-scale not describe the quasi-sinusoidal path of an isolated bright struc- structure of the corona during 2003 was neither as complex as ture rotating with the Sun. During the two weeks, the west-limb during solar maximum, nor as simple as during solar minimum streamer migrates slowly in the plane of the sky from -60◦ to - when streamers appear primarily at the equator. Choosing a 20◦ while the east limb streamer varies between 30◦ and 65◦. To relatively simple corona with isolated streamers at mid- to maintain such a slow variation, the structure of the north corona high-latitudes greatly facilitates the analysis of the large-scale is likely to be dominated by an extended longitudinal band of coronal structure. Figure 1D shows details of the large helmet high density. The synoptic maps shown for two heights in figure streamer seen on the north-west limb in figure 1A, in relation 2 are very similar, a result of the predominantly radial large- to the position of two prominences (the two northernmost white scale corona at this phase of the solar cycle. However, structures crosses) and an active region/prominence complex (white cross narrow considerably between 2.5 and 4.2R⊙, where the brightest near the equator) at the west limb, from which the legs of the central regions of the streamers are confined to very narrow lati- streamer seem to arise.
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