“Slow Solar Wind Sources and Acceleration Mechanisms in the Corona”

ISSI International Research Team project on

“Slow solar wind sources and acceleration mechanisms in the corona”

Team Leaders: Lucia Abbo (INAF/OATo, Italy) and Leon Ofman (CUA/NASA, USA) Date: 28 March 2013

Research Domain: Solar and Heliospheric Physics

Abstract: The main goal of this ISSI Team project is to merge observational and numerical modeling knowledge and expertise in order to investigate the sources of the Slow Solar Wind, the physical mechanisms at the base of its acceleration and the key role of the topology of the coronal magnetic field . Results from the ESA-NASA SOlar and Heliospheric Observatory (SOHO), -combined with theoretical modeling, have helped to investigate many aspects of the solar wind. Fundamental physical properties of the coronal plasma have been derived from SOHO/UVCS data and these results have provided crucial insights for a deeper understanding of the origin and acceleration of the slow solar wind (SSW). One of these was the discovery that quiescent streamers have a marked oxygen ion depletion in their cores with respect to their bright lateral branches. Furthermore, the elemental abundances (e.g. for Fe and O) vary among different coronal structures with respect to the photospheric values (this is the so called First Ionization Potential effect). Recently, it has been discovered that a core dimming is also apparent in the Mg X 62.5 nm line, even if less evident than for O VI 103.2 nm. Moreover, it has been found that a significant amount of slow solar wind originates outside the streamer/coronal hole boundaries, where the wind velocity depends on the magnetic field topology of flux tubes. Hence, it is fundamental to establish whether the physical parameters of the solar wind, such as outflow speed and energy deposition in the extended corona, are indeed modulated by the degree of expansion of the magnetic flux tubes channelling the wind through the corona. SOHO/LASCO white light coronagraphic observations provide critical evidence linking the solar-minimum streamer belt with the SSW: several small CMEs in the form of slow “streamer blowouts” were observed and they were considered as tracers of SSW. More recently, STEREO COR1/2 and HI data provided the velocity of small-scale propagating transients without projection effects, demonstrating the capability of STEREO instruments to monitor solar ejecta out to and beyond 1 AU. Recent results from the Hinode and SDO missions show persistent outflows at the edges of active regions whose contribution to the SSW is not completely understood. It remains to be determined what fraction of the SSW comes from the coronal hole/streamer interface and what part is produced by transient eruptions in coronal streamers. The Slow Solar Wind origin is now one of the outstanding questions arising in the post SOHO era and forms a major objective for planned future missions such as the Solar Orbiter and Solar Probe Plus. From a theoretical point of view, the ejection of material may be caused by loss of confinement due to pressure- driven instabilities as the heated plasma accumulates or due to current-driven instabilities (tearing and or kink-type instabilities) in the sheared field of the streamer. On small scales, 2.5-D magneto-hydrodynamic (MHD) models can account for the plasmoid blowouts observed in helmet streamers: these are due to magnetic reconnection at the current sheet above the cusp and are accelerated by a Kelvin-Helmholtz instability triggered by the reconnection itself. Multi-fluid 2.5-D models of the SSW have been developed to simulate streamers that contain heavy ions (in addition to protons and electrons), since traditional single fluid MHD models do not account for different properties and dynamics of various ions. Nevertheless, only very few multi-fluid studies of the SSW have attempted to reproduce the streamer observations by considering heavy ions. Due to their intrinsic complexity, so far kinetic models of the solar wind have been largely devoted to exploring the kinetic physics involved rather than offering direct detailed comparisons with observations. Hence we will mainly adopt a multi-fluid approach as the modeling component of our project. Today, there is an urgent need to integrate different expertise in the solar scientific community. On one hand, many coronal and solar wind models have ad-hoc and idealized boundary conditions at the Sun that coronal observations can otherwise help to constrain. On the other hand, it is often challenging to analyze coronal observations due to projection effects in the optically thin corona. In the latter case, numerical modelling can help to guide the determination of the 3D coronal structure. Unique and innovative results derived from this approach based on a synergy between observations and numerical modeling will provide an estimate of contributions to the SSW from different sources such as streamer boundary and streamer cusp and will quantify their role in the overall mass and energy budget of the SSW.

1 Scientific rationale of the project The solar wind is a continuous stream of charged particles (mainly electrons and protons, but also heavy ions) -14 ejected from the Sun at an average mass loss rate of (2 – 3)×10 Msun /year. Results from Ulysses and from the SOlar and Heliospheric Observatory (SOHO), two ESA-NASA space missions, combined with theoretical modeling, have helped in the understanding of many aspects of the solar wind. However, the heating and acceleration mechanism of the solar wind remains poorly understood. Ulysses with in situ measurements,, has clarified its 3-dimensional structure, demonstrating that there exists two principal components: a “slow” ( vslow ~ 300 – 400 km/s at 1AU) and a “fast” ( vfast ~700 – 800 km/s at 1AU) solar wind component, ejected during the minimum phase of the solar activity cycle from the low and high latitude regions, respectively (McComas et al., 2000). The processes that lead to the different fast and slow solar wind acceleration and properties have not yet been completely identified. It has been suggested that the geometry of magnetic field lines in the solar atmosphere determined at several heliocentric heights, could play a role in the fast wind acceleration (e.g. Munro & Jackson, 1977). There are also distinct pointers to other acceleration mechanisms, such as ion cyclotron resonance (Isenberg, 2001) or Alfvén wave acceleration mechanisms (see, Ofman 2010 for a review). During solar minimum, the low latitude Slow Solar Wind (SSW) at 1 AU can be traced back to source regions near equatorial coronal streamers. At least four possible source regions of SSW have been proposed concerning coronal streamers (Fig.1): (1) mixing of plasma inside the streamer/coronal hole boundaries, (2) plasma leakage from just one side in the core, just below the cusp, (3) quasi-steady flow from the legs of streamers, and (4) parcels of plasma escaping from the core, carrying loops of magnetic flux (e.g. see Suess et al. 2009). Crucial results on the origin of the solar wind have been derived not only from in- situ measurements, but also from remote sensing techniques . During the last 17 years two coronagraphs, the Large Angle and Spectrometric Coronagraph ( LASCO ; Brueckner et al., 1995) and the Ultraviolet Coronagraph Spectrometer ( UVCS ; Kohl et al., 1995) onboard SOHO, have acquired data of the extended corona. LASCO white light observations provided evidence Fig.1: Four possible sources of slow wind (Suess et al. 2009). linking the solar-minimum streamer belt with the SSW. For example, Sheeley et al. (1997) used LASCO C2 to observe several small eruptions in the form of slow “streamer blowouts” which are widely believed to be tracers of SSW. Mierla et al. (2007) have obtained SSW outflow speeds of 10-20 km/s at 1.3 R sun using LASCO C1 data. UVCS spectroscopic observations have significantly contributed to our understanding of streamers since the beginning of the SOHO mission. The main results derived from UVCS observations of coronal streamers and the SSW wind can be summarized as follows (see also Antonucci 2006 and Kohl et al. 2006 for reviews of UVCS results): • Streamer core oxygen depletion: Previous studies of streamers at solar minimum based on UVCS data have revealed an abundance anomaly (e.g. Noci et al. 1997, Marocchi et al. 2001, Uzzo et al. 2003) that might be related to the origin of the low-speed streams. Quiescent streamers show depletion in O VI emission in the core with respect to their bright lateral branches (Fig. 2). Several different explanations for this feature have been proposed (e.g. Noci et al. 1997; Raymond et al. 1997; Ofman 2000; Frazin et al. 2003; Akinari, 2007). • Streamer elemental composition: Elemental abundances vary among the different coronal structures with respect to photospheric values. The determining parameter appears to be the First Ionization Potential (FIP) of different elements (i.e., the FIP-effect). This effect is much more pronounced in the SSW than in the fast solar wind (von Steiger et al. 2000) and therefore it can be very useful as a tracer of their sources. A quantitative analysis that includes the reduction of the drag force (due to differential proton-ion speeds) on the different ion species (Geiss 1982; Geiss et al. 1995) would be necessary to assess the relationship between wind speed and the relative enhancement in the low FIP elements. Ko et al. (2008) provided maps of coronal plasma physical parameters of streamers derived from observations that were compared with large-scale coronal properties of a 3D MHD model. • SSW and flux tube expansion factors: Strachan et al. (2012) used synoptic maps of electron density and coronal outflow velocity at ~2.5 Rsun to estimate flux tube expansion factors, fexp , as a function of latitude at solar minimum. The novelty of this work shows that flux tube expansion factors can be determined from the physical conditions in the corona, independent of magnetic field measurements. Preliminary results show that large f exp are found at the edges of streamers where the SSW is thought to originate. Antonucci, Abbo & Telloni (2012) also found that, during solar minimum, when the coronal magnetic configuration is rather simple, the open magnetic fields emerging from the wide polar coronal holes channel both the fast and the slow wind: the fast wind flows along flux tubes with lower areal divergence than in the slow wind which is guided by flux tubes characterized by non-monotonic areal expansion functions. 2 • SSW origin: By applying Doppler dimming analysis based on the ratio of O VI line intensities (see Noci et al. 1987), it has been shown that equatorial streamers at solar minimum exhibit plasma outflows beyond 3.6 R sun along the streamer axis (Strachan et al. 2002; Susino et al. 2008). Indeed, Noci & Gavryuseva (2007), by determining a lower limit of the outflow speed derived from the O VI line ratios in the streamer region, found that SSW directly emerging from the streamers are likely confined to a thin layer near the current sheet. Abbo et al. (2010a) found that the main source for the slow solar wind is the coronal hole/streamer boundary region. They adopted an improved version of the Doppler dimming technique (Antonucci et al. 2004) that is used to derive both electron density and outflow velocity of the expanding corona from the O VI λλ 103.2-103.7 nm line intensities, given constraints on the geometry of flow tubes connecting corona and heliosphere. Moreover, Abbo et al. (2006) found that open magnetic field regions outside streamers are characterized by oxygen abundance (relative to hydrogen) typical of those from the heliospheric SSW. More recent results from the EUV Imaging Spectrometer (EIS) and the X-ray Telescope (XRT) on board the Hinode satellite show persistent outflows at the edges of active regions and extended large-scale loops emanating along open magnetic field lines into the upper Fig.2: UVCS observations of an equatorial solar corona, indicating a possible SSW source (Sakao et al. minimum streamer in HI- Lya (top-right) and OVI 2007; Harra et al. 2008). Interesting results have also been 103.2 nm emission (bottom right) and found from the STEREO mission: data acquired by COR1 corresponding results from 2.5D multi-fluid model and the Heliospheric Imagers (HI) show that a plethora of (left panels, from Ofman, Abbo & Giordano, 2011) . ascending coronal features (probably connected to the same inhomogeneities observed by LASCO at lower altitudes) propagate within the solar wind out to and beyond 1 AU (Davies et al., 2009; Jones and Davila, 2009; Wang 2012). Nevertheless , it remains to be determined what fraction of the SSW comes from each of these possible contributions . There are indications, as suggested by the SOHO observations, that the SSW is a combination of a highly fluctuating component and quasi-stationary flow coming from the equatorial streamer belt. Dynamical simulations of the regions of SSW formation are particularly challenging due to the need to include the effects of changing magnetic field topology and also of the formation of plasma inhomogeneities. The intermittent contribution can be explained as due to magnetic reconnection at the cusp of the streamer. In such a case, magneto-hydrodynamic (MHD) models indicate that small eruptions at the helmet streamer cusp may continually accelerate small amounts of plasma (e.g. Einaudi et al., 1999). This model has been improved by including the effects due to curvature and expansion in a spherical geometry (Rappazzo et al. 2005). Also, the effect of converging flows has been analyzed by Lapenta & Knoll (2005) and Lapenta & Restante (2008) focusing also on the effect of viscosity on the overall system. Wiegelmann et al. (2000) indicated that small eruptions at the helmet streamer cusp may incessantly accelerate small amounts of plasma without significant changes of the equilibrium configuration of multiple sub-streamers. A model of a two component SSW has been proposed by Wang et al. (2000): one component flowing along the rapidly diverging open magnetic field lines adjacent to the streamer boundary, and the second one confined to the region of the denser equatorial plasma sheet. Other Fig.3: Example of magnetic field useful models include a 3-D MHD single fluid polytropic model of the lines map calculated by the 3D-MHD global corona (see Mikic et al. 1999, Fig. 3). This model has been model by Mikic et al. (1999), improved by Lionello et al. (2009) to reproduce EUV and X-ray showing the structure of the open- observed coronal emissions and by Riley et al. (2012) to interpret the and closed- field regions. interplanetary signatures of unipolar streamers (also known as pseudo- streamers). Models, such as those developed by Antiochos et al. (2007, 2011) suggest that the source of the slow wind at the Sun is a network of narrow open-field corridors that map to a web of quasi-separatrix layers in the 3 heliosphere. An interesting review about the solar wind models from the chromosphere up to the heliosphere has been published by Hansteen and Velli (2012). Two-dimensional multi-fluid models of the SSW have been developed as well: Ofman (2000; 2004; et al. 2011; 2013) describes electrons, protons and heavy ions (O5+ and Mg 9+ ) as coupled fluids in a 2.5 D multi-fluid model and different heating mechanisms are considered for each species. This model successfully recovers the basic features of solar streamers, as well as the acceleration and heating profiles for protons and heavy ions (Li et al. 2006, Abbo, Ofman & Giordano 2010b , Ofman, Abbo & Giordano, 2011; Ofman, Abbo & Giordano, 2013). The heating and acceleration of slow solar wind by observationally constrained semi-empirical heating function were investigated in 2.5D MHD model (Airapetian et al 2011) and show that the slow solar wind is consistent with a thermal pressure gradient driven wind originally proposed by Parker. Despite the progress described above, present numerical models alone are not able to determine unambiguously what the primary source(s) of SSW is (are). This determination requires a strict combination of multi-wavelength coronal observations along with the use of improved modeling. The results from the proposed work will feed directly into answering the major science goals for two future missions: Solar Orbiter and Solar Probe Plus.

Scientific goals and objectives The main goal of this project is to answer the following question: What are the source regions for different contributions of SSW and how do they operate? In order to answer this question, we will propose an International Team of experts to address the following related sub-objectives: • Identify possible mechanisms for the differences in elemental abundances within coronal streamers and the surrounding regions, and their contribution in the abundance variation in the SSW • Understand elemental abundance depletions in the core of some streamers, and their contribution as a possible source of the SSW • Investigate the key role of the magnetic topology of coronal streamers where SSW is formed and accelerated and where the energy is released • Identify (or at least reduce the number of) possible acceleration and heating mechanisms for the SSW.

These goals will be addressed by using an iterative approach that compares the empirical results from observations with results from numerical models developed by our team members. Multi-spacecraft observations using remote sensing instruments (e.g. SOHO/EIT, LASCO, SUMER, UVCS; HINODE/EIS; SDO/AIA) and in- situ instruments on Ulysses, ACE, and WIND will be used to provide estimates of the plasma parameters (density, temperatures, outflow velocities and abundances) in the SSW formation regions. Photospheric magnetic field measurements (using ground- and space-based magnetograms) will be used to drive MHD and multi-fluid models that simulate both the plasma and magnetic field geometry of coronal streamers and their surrounding regions. We will construct direct observables from the models and compare these with SSW signatures identified from the observations by velocity and abundance diagnostics. In cases where the observations and models disagree, the models will be modified in order to better match the coronal observations. The model parameters we eventually arrive at will allow us to tell quantitatively how much each potential source contributes to the overall SSW mass budget. Empirical models that are used to produce the streamer plasma parameters from observables can also be improved by using, for example, the steady state magnetic fields predicted by MHD models. Due to their intrinsic complexity, so far kinetic models of the solar wind have been largely devoted to exploring the kinetic physics involved rather than offering direct detailed comparisons with observations. Hence we will mainly adopt a multi- fluid approach as the modeling component of our project. Because of the complexity of the various models (theoretical and empirical), face-to-face meetings are crucial for identifying issues and undertaking consistent simulations. The innovative results that will be achieved from this approach are based on a synergy between observations and numerical modeling, and will provide a robust estimate of contributions to the SSW from different sources. Additionally, they will shed light on their role in the overall mass and energy budget of the SSW. The proposed project will involve scientists from Belgium, China, Italy, Norway, Switzerland, United Kingdom and United States of America (see the list of team members and Appendix A).

Timeliness of the project The Origins of the Solar Wind is one of the major open questions in solar physics. For this reason it is listed as a highest-priority scientific objective for both Solar Orbiter and Solar Probe Plus. In anticipation for these new solar missions, the proposed project will lay a solid foundation for fostering the type of close collaboration between observers and modelers that is needed to make progress on this problem. Although the present project will not have the near-Sun in-situ data from these future missions, much can be gained by using the currently available data with more powerful coronal models that are currently being developed. Remote sensing (spectral and imaging) observations will provide the constraints (see the previous section) for the physical conditions in coronal streamers.

4 It is desirable to complete this project early enough so that its results can feed into the development of new observing programs and data analysis plans for these upcoming missions.

Expected outcomes This work is intended to bring studies of the SSW onto an equal footing with our present understanding of the fast solar wind, making significant progress in identifying and characterizing SSW source regions. Our aim is to efficiently combine research efforts and to develop models that will help identify the most likely physical processes in SSW source regions. The project results will be presented at international conferences and published in internationally recognized journals. The following refereed publications are anticipated from the project: • A review article on recent observational results and on 2.5D and 3D MHD modeling results of the slow solar wind. • One or more articles describing how to combine the observational results with the different multi-fluid models of SSW acceleration and heating ISSI support will be acknowledged in all of the above publications. The Team Leaders will also setup a website for the project that will describe the following: the aims of the project, the membership of the Team, the project schedule and the latest scientific results.

Reasons for choosing ISSI as implementation site: 1) Opportunity to focus on a specific field of research in an international environment: Experts in this field are located all over the world, which presents an obstacle to making progress in this field. Establishing a collaboration among scientists with different expertise and different approaches will strengthen the multidisciplinary aspects of the research we are proposing and result in a deeper understanding of the issues; 2) Excellent facilities and reputation: ISSI represents an excellent common ground to bring the U.S. and European communities together and to have theorists interact with observers and share problems while sitting at the same table; 3) The city of Bern and its central location (within Europe) ; 4) Financial support for the Team. Most of our team members have participated in previous ISSI teams and appreciate the importance of the ISSI environment in allowing small groups of experts with common interests to make significant progress on a focused topic and to foster fruitful collaborations.

List of confirmed participants (alphabetical order) 1) Abbo, Lucia, INAF-Osservatorio Astrofisico di Torino, Pino Torinese (TO), Italy 2) Antiochos, Spiro K., NASA-GSFC, Greenbelt, MD, USA 3) Hansteen, Viggo H., Institute of Theoretical Astrophysics, University of Oslo, Oslo, Norway 4) Harra, Louise, UCL-Mullard Space Science Laboratory, Dorking, Surrey, UK 5) Ko, Yuan-Kuen, Space Science Division, Naval Research Laboratory, Washington, DC, USA 6) Lapenta, Gianni, Centre for Plasma Astrophysics, Leuven, Belgium 7) Li, Bo, School of Space Science and Physics, Shandong University, Weihai, PR China 8) Riley, Pete, Predictive Science, Inc., San Diego, CA, USA 9) Ofman, Leon, Catholic University of America, NASA-GSFC, Greenbelt MD, USA 10) Strachan, Leonard, Harvard - Smithsonian Center for Astrophysics, Cambridge, MA, USA 11) von Steiger, Rudolf, International Space Science Institute, Bern, Switzerland 12) Wang, Yi-Ming, Space Science Division, Naval Research Laboratory, Washington, DC, USA

Schedule of the Project There is request for the support of two Team Meetings at ISSI of one-week duration, each. 1st meeting : February- March 2014; 2nd meeting : February-March 2015. Completion of the project: May-June 2015.

Facilities required The standard ISSI workshop facilities are required, i.e. a meeting room for 18 people (12 team members + 3 students/young scientists + 3 external experts), equipped with data projection facilities, wireless internet access and some limited printing facilities. We expect that most team members will use their own laptop computers. In addition, we would ask a room to arrange one-day splinter Meetings.

Financial support requested to ISSI We request that ISSI provide living expenses ( per diem and accommodation) for 12 team members, two times for 5 days. Travel costs of the Team Leaders (train transfer Turin-Bern, R/T airfare Washington, DC - Bern) are also requested, while all other Team members will be responsible for their travel to ISSI.

5 Appendix A Addresses, telephone, fax, and e-mail of all team members

BELGIUM Lapenta, Gianni Centre for Plasma Astrophysics, K. U. Leuven Celestijnenlaan 200b- bus 2400, 3001 Leuven, Belgium, [email protected] Tel: +32-16-327965 Fax: +32-16-327998

CHINA Li, Bo Shandong Provincial Key Laboratory of Optical Astronomy & Solar-Terrestrial Environment, School of Space Science and Physics, Shandong University at Weihai, 180 West Wenhua Road, 264209 Weihai, PR China, [email protected] Tel: +86-631-5673527 Fax: +86-631-567 3578

ITALY Abbo, Lucia INAF-Osservatorio Astrofisico di Torino, via Osservatorio 20, 10025 Pino Torinese (TO), Italy, [email protected] Tel: +39-011-8101954 Fax: +39-011-8101930

NORWAY Hansteen, Viggo H. Institute of Theoretical Astrophysics, University of Oslo, PB 1029, Blindern N-0315, Oslo, Norway, [email protected] Tel: +47-22856120 Fax: +47-22856505

SWITZERLAND von Steiger, Rudolf Director, International Space Science Institute, Hallerstrasse 6 3012 Bern Switzerland, [email protected] Tel: +41-31-631-48-90 Fax: +41-31-631-48-97

UNITED KINGDOM Harra, Louise UCL-Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK, [email protected] Tel: +44-1483-204141 Fax: +44-1483-278312

USA Antiochos, Spiro K. NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA, spiro.antiochos@nasa.gov Tel: +1-301-286-8849 Fax: +1-301-286-9203

6

Ko, Yuan-Kuen Space Science Division, Naval Research Laboratory, Washington, DC 20375-5352, USA, [email protected] Tel: +1-202-767-6199 Fax: +1-202-404-7997

Riley, Pete Predictive Science, Inc., 9990 Mesa Rim Road, Suite 170, San Diego, CA 92121, USA [email protected] Tel: +1-858-450-6488 Fax: +1-858-408-1953

Ofman, Leon Catholic University of America, NASA-Goddard Space Flight Center, Code 671, Greenbelt, MD 20771, USA, [email protected] Tel: +1-301-286-9913 Fax: +1-301-286-1617

Strachan, Leonard Harvard - Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA, [email protected] Tel: +1-617-496-7569 Fax: +1-617-495-7049

Wang, Yi-Ming Space Science Division, Naval Research Laboratory, Washington, DC 20375-5352, USA [email protected] Tel: +1-202-404-8460 Fax: +1-202-404-7997

7 Appendix B Brief CVs of all team members

Abbo Lucia INAF-Osservatorio Astrofisico di Torino via Osservatorio 20, 10025 Pino Torinese (TO) , Italy Tel: +39-011-8101-954 Fax: +39-011-8101-930 email: [email protected]

Dr. L. Abbo has 13 years’ experience in the scientific analysis of solar data. She has been member of two Scientific Team at ISSI (Bern). She has been Lead Scientist at NASA Goddard Space Flight Center, Greenbelt (USA), for planning observations and acquisition data of the UVCS instrument on board SOHO and also during several observational Campaigns at the Multi-Experiment Data Operation Centre (IAS, France). She is co-I of the METIS coronagraph for ESA Solar Orbiter mission. She is Associate Scientist of the project entitled "The origin of the slow solar wind", with PI prof. Leon Ofman accepted in February 2011 in the program Living With a Star Targeted Research and Technology. She has been coordinator of the Intercalibration Program (ICAL) 14 entitled "SOHO-STEREO-TRACE-HERSCHEL radiometric cross-calibration". Her main research interests in solar physics are: EUV Spectroscopy of the Solar Corona and Solar Wind; determination of physical parameters of Coronal Structures such as Streamers and Coronal Holes through developing diagnostic techniques of coronal plasma by considering the magnetic topology of the magnetic field; spectroscopic study of the supergranulation in chromosphere and transition region; data reduction, analysis and interpretation of SOHO/UVCS, SUMER, MDI, CDS; HINODE/EIS, SOT; SDO/AIA, HMI. Positions Held Since 2007 Research Astronomer – National Institute of Astrophysics (INAF)/Turin Astrophysical Observatory (OATo), Pino Torinese, Italy 2005-2007 Post-doctoral fellow – INAF/OATo, Pino Torinese, Italy 2004 Post-doctoral fellow - Institut d’Astrophysique Spatiale, Orsay, France

Education University of Turin, Italy 2003 Ph.D. in Physics. Thesis: " Identification of the Coronal Sources of the Slow Solar Wind" 1999 Graduate Degree in Physics, with honors

Selected Publications • Ofman, L., Abbo, L., Giordano, S., 2013, “Observations and models of slow solar wind with Mg 9+ ions in quiescent streamers”, ApJ, 762, 18 • Gabriel, A.H., & Abbo, L., 2012, “ Outflow velocity structure in the upper transition region and corona” , Sol. Phys., 280, 2, 435 • Ofman, L., Abbo, L., Giordano, S., 2011, “ Multi-fluid Model of a Streamer at Solar Minimum and Comparison with Observations” , ApJ, 734, 30 • Antonucci, E., Abbo, L., Telloni, D., 2011, “UVCS Observations of Temperature and Velocity Profiles in Coronal Holes” , Space Science Reviews,172, 1, 5 • Wilhelm, K., Abbo, L., Auchère, F., et al. 2011, “Morphology, dynamics and plasma parameters of plumes and interplume regions in solar coronal holes”, A&A Rev., 19, 1, 35 • Abbo, L., Antonucci, E., Mikic, Z., et al. 2010, “Characterization of the slow wind in the outer corona” , Adv. Space Res., 46, 11, 1400 • Abbo, L., Ofman, L. & Giordano, S. 2010, “Streamers study at solar minimum: combination of UV observations and numerical modeling” , Proc. of the Solar Wind 12, AIP Conf. Proc., 1216, 387 • Antonucci, E., Abbo, L. & Telloni, D. 2006, “Oxygen abundance and energy deposition in the slow coronal wind” , ApJ, 643, 1239 • Abbo, L. et al. 2006, “Slow coronal wind composition” , ESA SP-617 • Antonucci, E., Abbo, L. & Dodero, M.A. 2005, “Slow wind and magnetic topology in the solar minimum corona in 1996-1997” , A&A, 435, 699

8 Ofman Leon Catholic University of America, NASA-GSFC, Greenbelt, MD, USA Tel: +1-301-286-9913 Fax: +1-301-286-1617 email: [email protected]

Education and Experience Prof. Leon Ofman received his B.Sc. in Physics in 1986 and M.Sc. in Physics in 1988 from Tel Aviv University, Israel, and his Ph.D. in Physics in 1992 from the University of Texas at Austin. He held National Research Council Postdoctoral Research Associateship at NASA Goddard Space Flight Center from 1992 to 1994. Since 1994 Prof. Ofman continued working at NASA GSFC, as a contractor via Hughes and Raytheon corporations, and in 2001 he became a Research Associate Professor at Catholic University of America, Associate Professor (2005-2007), and a University Affiliate (contractor) at NASA GSFC to present. From 2007 Prof. Ofman became Visiting Associate Professor at Tel Aviv University. In 2009 Prof. Ofman became Research Professor at CUA’s Department of Physics and Institute for Astrophysics and Computational Sciences (IACS). His main research interests are in solar plasma physics, Magnetohydrodynamics, waves and instabilities, and kinetic processes related to coronal heating and acceleration of the solar wind. His main expertise is in numerical modeling of the solar coronal and wind plasma, driven by space based observations. Prof. Ofman has authored and coauthored 147 publications in solar physics and related fields in refereed journals, and in conference proceeding. Prof. Ofman is the Principal Investigator on NASA and NSF grants supervising postdocs and a student at NASA GSFC that work in solar physics. Prof. Ofman was a member of NASA Science Definition Team for the Solar Probe Plus mission. He is serving as a referee for leading journals in the field, and a reviewer for NASA, NSF, and other agencies. Prof. Ofman is a member of American Astronomical Society - Solar Physics Division, American Geophysical Union, International Astronomical Union, Committee on Space Research, and Asia and Oceania Geosciences Society.

Selected Recent Publications: • Ofman, L., Abbo, L., and Giordano, S., Observations and models of slow solar wind with Mg9+ ions in quiescent steamers, ApJ, 762, 18, 2013. • Ofman, L., Viñas, A.-F., and , Moya, P.S., Hybrid models of solar wind plasma heating, Annales Geophysicae, 29, 1071, 2011. • Ofman, L., Abbo, L., and Giordano, S., Multi-fluid model of a streamer at solar minimum and comparison with observations, The Astrophysical Journal, 734, 30, 2011. • Airapetian, V., Ofman, L., Sittler, E.C., and Kramar, M., Probing Thermodynamics and Kinematics of Solar Coronal Streamers, The Astrophysical Journal , 728, 67, 2011. • Ofman, L., Wave Modeling of the Solar Wind, Living Rev. Solar Phys., 7, 4, URL: http://solarphysics.livingreviews.org/Articles/lrsp-2010-4, 2010. • Ofman, L., Hybrid model of inhomogeneous solar wind plasma heating by Alfven wave spectrum: parametric studies, Journal of Geophysical Research , 115, A04108, doi:10.1029/2009JA015094, 2010. • Ofman, L., Progress, challenges, and perspectives of the 3D MHD numerical modeling of oscillations in the solar corona, Space Science Rev. , doi: 10.1007/s11214-009-9501-1, 2009. • McComas, D.J., Velli, M., Lewis, W.S., Acton, L.W., Balat-Pichelin, M., Bothmer, V., Dirling, R.B., Jr., Feldman, W.C., Gloeckler, G., Habbal, S.R., Hassler, D.M., Mann, I., Matthaeus, W.H., McNutt, R.L., Jr., Mewaldt, R.A., Murphy, N., Ofman, L., Sittler, Jr., E.C., Smith, C.W., and Zurbuchen, T.H., Understanding coronal heating and solar wind acceleration: the case for near- sun measurements, Reviews of Geophysics, 45, RG1004, doi:10.1029/2006RG000195, 2007.

9 Antiochos Spiro Kosta NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Tel: +1-301-286-8849 Fax: +1-301-286-9203 email: [email protected]

BA McGill University, 1970 PhD Stanford University, 1976

Biography

Since January 2008, Dr. Antiochos has been a senior scientist in the Heliophysics Division of NASA GSFC. Since January 2003, Dr. Antiochos has also been an Adjunct Professor in the Department of Atmospheric, Oceanic, and Space Sciences at the University of Michigan. His fields of expertise include theoretical solar physics and plasma physics. His work consists primarily of developing theoretical models to explain observations, and relies heavily on magneto-hydrodynamic (MHD) theory, especially nonlinear equilibria and instabilities, and on large-scale numerical simulations. During his career he has worked on a number of problems related to the Sun and Heliosphere, in particular, the physics of magnetic driven activity and heating, and the structure of the solar corona and transition region. Some of his most widely recognized contributions are his work on cool loop models for the transition region, on the thermal non-equilibrium model for coronal condensations, on the 3D sheared arcade model of prominence magnetic fields, and on the “breakout” model for coronal mass ejections and eruptive flares.

From June 1985 – December 2007, Dr. Antiochos was an Astrophysicist in the Space Science Division of NRL. From April 1980 – June 1985, Dr. Antiochos was a Senior Research Associate at the Center for Space Science and Astrophysics at Stanford University. From May 1978 – April 1980, Dr. Antiochos was a Research Associate at the Institute for Plasma Research at Stanford University. From October 1976 – April 1978, Dr. Antiochos held a Skylab Post-Doctoral Fellowship with the National Center for Atmospheric Research in Boulder Colorado.

Dr. Antiochos is a member of the American Geophysical Union (AGU), the American Astronomical Society (AAS), the American Physical Society, and the International Astronomical Union. He has served on many advisory/review committees including Chair of the Solar Physics Division of the AAS, Chair of the NASA Solar Management and Operations Working Group, Chair of the SOLAR-B Science Definition Team, and member of the Space Studies Board of the National Research Council. Dr. Antiochos has been elected Fellow of the AGU and the APS and Honorary Fellow of the Royal Astronomical Society, and has been awarded the George Ellery Hale Prize by the AAS and the E. O. Hulburt award by NRL.

Selected Bibliography • “Reconnection onset and eruption takeoff in the breakout model for coronal mass ejections,” J. T. Karpen, C. R. DeVore, and S. K. Antiochos, 2012, ApJ, submitted. • “A model for the sources of the slow solar wind,” S. K. Antiochos, Z. Miki ć, R. Lionello, V. S. Titov, and J. A. Linker, 2011, ApJ, 731, 112. • “Formation and dynamics of three-dimensional current sheets in the solar corona,” J. K. Edmondson, S. K. Antiochos, C. R. DeVore, and T. H. Zurbuchen, 2010, ApJ, 718, 72. • “Three-dimensional modeling of quasi-homologous solar jets,” E. Pariat, S. K. Antiochos, and C. R. DeVore, 2010, ApJ, 714,762.

10 Hansteen Viggo H. Institute of Theoretical Astrophysics, Univ. of Oslo PB 1029, Blindern N-0315,Oslo,Norway Tel: +47-22856120 Fax: +47-22856505 email: [email protected]

Professor at the Institute of Theoretical Astrophysics, University of Oslo

Research Interests Main research area relate to dynamics and heating of outer solar atmosphere using both observational and numerical techniques.

Education

• 1992 : Dr. Scient from the University of Oslo, Institute of Theoretical Astrophysics (ITA) • 1988 : Cand. mag. 1988 from University of Oslo

Employment

• 04.84-12.86 : Student Assistant at Oslo Solar Observatory • 01.87-12.88 : Research Assistant at ITA • 01.89-08.92 : Doctoral Research Assistant at ITA • 02.92-08.92 : Visiting Scientist at High Altitude Observatory, Boulder CO • 08.92-10.95 : Research Fellow at ITA • 10.94-10.95 : Visiting Scientist at High Altitude Observatory, Boulder CO • 11.95-04.97 : Førsteamanuensis at ITA • 05.97- : Professor at ITA • 07.02-07.02 : Visiting Scientist at Mullard Space Science Lab., Holmsbury, Surrey • 02.06-04.06 : Visiting Scientist at Lockheed Martin Space and Astrophysics Lab, Palo Alto CA • 07.09-08.09 : Visiting Professor at National Astronomical Observatory of Japan, Tokyo

Experience

Vice Director of the Institute of Theoretical Astrophysics 1997-2008. Norwegian coordinator for the EU network “Solaire”, 2007-2011. Norwegian coordinator for the EU network “Theory, Observations and Simulations of Turbulence in Space Plasmas”, 2002-2005. Head of the Norwegian Hinode (Solar-B) project, 1998– Participant in the Centre of Excellence “Centre of Mathematics for Applications”, 2003–2012 Member of the Solar System Working Group, ESA, 2004–2007. ESA representative to the “Hinode Science Working Group”, 2007–

11 Harra Louise UCL-Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK Tel: +44-1483-204141 Fax: +44-1483-278312 email: [email protected]

EDUCATION Queens University, Belfast, N.Ireland October 1990 - August 1993 • Ph.D Physics August 1993 "Spectroscopic Diagnostics for Solar and Laboratory Plasmas" • BSc(Hons) Applied Maths and Physics June 1990

PROFESSIONAL HISTORY UCL Department of Space and Climate Physics Mullard Space Science Laboratory, Holmbury St Mary, Dorking, Surrey, UK. RH5 6NT

Professor of Solar Physics 2006 – present

Head of Solar and Stellar Physics September 2012 to present

OTHER CURRENT MAJOR APPOINTMENTS AND AFFILIATIONS PI of the Hinode EIS instrument (2006-present) Co-PI of EUV Imager on Solar Orbiter (2009-present) Instrument selected in 2009. Selection committee for National Solar Observatory director, 2012 Member of UKSA’s space projects review panel (2011-) Member of the remote sensing working group for Solar Orbiter (2011- ) Member of international Solar-C EUV/VUV spectroscopy sub-WG (2009- ) Vice-chair for COSPAR sub-commission E2/D3 (interdisciplinary) (2004 to present) Partner in UCL’s centre for space medicine, 2012- present

PUBLICATIONS (143 refereed papers) • Harra, L.K., Archontis, V., Pedram, E., Hood, A. W., Shelton, D. L. and van Driel-Gesztelyi, L.,”The Creation of Outowing Plasma in the Corona at Emerging Flux Regions: Comparing Observations and Simulations”, Solar Phys., 2012, 278, 47 [1] • Harra, L.K., Sterling, A.C., G
om
ory, P., Veronig, A., ”Spectroscopic observations of a coronal Moreton wave”, ApJ Letters, 2011, 737, 4 [9] • Harra, L.K., Mandrini, C.H., Dasso, S., Gulisano, A.M and Steed, K. “Determining the Solar Source of a Magnetic Cloud Using a Velocity Difference Technique”, Solar Physics, 2011, 268, 213. [5] • Harra, L.K., Magara, T., Hara, H., Tsuneta, S., Okamaoto, T.J. and Wallace, A.J.,”Response of the Solar Atmosphere to the Emergence of `Serpentine' Magnetic Field”, Solar Phys, 2010, 263, 105. [11] • Harra, L.K., Williams, D.R., Wallace, A.J., Magara, T., Hara, H., Tsuneta, S., Sterling, A.C. and Doschek, G.A.,” Coronal Nonthermal Velocity Following Helicity Injection Before an X-Class Flare,” ApJL, 2009, 691, 99. [12] • Harra, L. K., Sakao, T., Mandrini, C. H., Hara, H., Imada, S., Young, P. R., van Driel-Gesztelyi, L., Baker, D.,”Outflows at the Edges of Active Regions: Contribution to Solar Wind Formation?”, ApJ, 2008, 676, 147. [63]

12 Ko Yuan-Kuen Space Science Division, Naval Research Laboratory Washington, DC 20375, USA Tel: +1-202-767-6199 Fax: +1-202-404-7997 Email: [email protected]

EDUCATION Ph.D., Physics, 1993, University of Maryland at College Park B.S., Physics, 1983, National Tsing-Hua University, Taiwan, Republic of China

PRIMARY RESEARCH INTERESTS Solar physics – spectroscopic diagnostics of the solar atmosphere and solar eruptive events Heliophysics – studies of solar wind formation, studies of variation in solar energetic particles

RECENT POSITIONS HELD Apr. 2008 – present, Astrophysicist, Naval Research Laboratory Feb. 1998 – Mar. 2008, Astrophysicist, Harvard-Smithsonian Center for Astrophysics Sep. 1994 – Feb. 1998, Assistant Research Scientist, Department of Atmospheric, Oceanic and Space Sciences, University of Michigan

SELECTED PUBLICATIONS - “On the Solar Wind Ion Composition and their Source Coronal Holes I. Low-Latitude Extension of Polar Coronal Holes”, Ko, Y.-K., Muglach, K., Wang, Y.-M., Young, P. R., Lepri, S. T., Laming, J. M., & Popecki, M., 2013, in preparation - “Heavy Ion Properties in ICMEs and Signatures of Magnetic Reconnection in Post-CME Current Sheet”, Ko, Y.-K., Raymond, J. C., Rakowski, C., & Rouillard, A. 2012, SW13 Conference Proceedings, in press - “On the Relationship Between Heavy-Ion Composition Variability in Gradual SEP Events and the Associated IMF Source Regions”, Ko, Y.-K., Tylka, A. J., Ng, C. K., & Wang, Y.-M. 2012, AIP Conf. Proc. 1500, 26 (2012); doi: 10.1063/1.4768740 - “Modeling UV and X-Ray Emission in a Post-CME Current Sheet”, Ko, Y.-K., Raymond, J. C., Vrsnak, B., & Vujic E. 2010, ApJ, 722, 625 - “Quiescent Current Sheets in the Solar Wind and Origins of Slow Wind”, Suess, S. T., Ko, Y.-K., von Steiger, R., Moore, R. L., 2009, JGR, vol.114, A04103, doi:10.1029/2008JA013704 - “Slow Solar Wind From Open Regions With Strong Low-Coronal Heating”, Wang, Y.-M., Ko, Y.-K., Grappin, R., 2009, ApJ, 691, 760 - “Hot Plasma in Non-Flaring Active Regions Observed by the Extreme-ultraviolet Imaging Spectrometer on Hinode”, Ko, Y.-K., Doschek, G. A., Warren, H. W., Young, P. R., 2009, ApJ, 697, 1956 - “Large Scale Coronal Density and Abundance Structures, and Their Association With the Magnetic Field Structure”, Ko, Y.-K., Li, J., Riley, P., Raymond, J. C., 2008, ApJ, 683, 1168 - “Abundance Variation at the Vicinity of an Active Region and the Coronal Origin of the Slow Solar Wind”, Ko, Y.-K., Raymond, J. C., Zurbuchen, T. H., Riley, P., Raines, J., Strachan, L. 2006, ApJ, 646, 1275 - “Dynamical and Physical Properties of a Post-Coronal Mass Ejection Current Sheet”, Ko, Y.-K., Raymond, J. C., Lin, J., Lawrence, G., Li, J., Fludra, A. 2003, ApJ, 594, 1068 - “Elemental Abundances for the 1996 Streamer Belt”, Uzzo, M., Ko, Y.-K., Raymond, J. C., Wurz, P., Ipavich, F. M., 2003, ApJ, 585, 1062 - “SOHO/UVCS and Yohkoh/SXT Observation of a High Temperature Corona Above an Active Region Complex”, Ko, Y.-K., Raymond, J. C., Li, J., Ciaravella, A., Michels, J.,Fineschi, S., Wu, R., 2002, ApJ, 578, 979 - “Solar wind ionic charge states during the Ulysses pole-to-pole pass”, Ko, Y.-K., Gloeckler, G., Cohen, C. M. S., Galvin, A. B., 1999, JGR, 104, 17005, DOI10.1029/1999JA900112 - “An Empirical study of the electron temperature profile and heavy ion velocities in the south polar coronal hole”, Ko, Y.-K., Fisk, L. A., Geiss, J., Gloeckler, G., Guhathakurta, M., 1997, Solar Physics , 171, 345

13 Lapenta Giovanni Centre for Plasma Astrophysics, 3001 Leuven, Belgium Tel: +32-16 327965 Fax: +32-16 327998 email: [email protected]

Master Degree in Nuclear Engineering at the Politecnico di Torino, February 1990. Ph.D. in Plasma Physics at the Politecnico di Torino, September, 1993. Visiting Scientist at the Massachusetts Institute of Technology and at Los Alamos National Laboratory (LANL) from 1992 to 1994. Director's Postdoctoral Fellow at LANL from 1994 to 1996. Tenured Research Professor of Computational Physics at Politecnico di Torino, 1996-2000. Technical Staff Member at LANL, 1998-2008. Professor of Space Weather, Katholieke Universiteit Leuven, Belgium, since January 2007.

Lapenta's research is currently focused on the study of various aspects of space weather and of solar, space and astrophysical systems. Lapenta’s expertise is in the development and use of theoretical and simulation tools for different problems in plasma physics. Lapenta is also involved in applying theoretical and simulation tools to the interpretation of experimental and observational findings. Lapenta is also involved in plasma and radiation physics research with application to laboratory and industrial systems.

Lapenta has been involved in large research efforts in USA and in Europe, as principal investigator and as co-investigator. Examples are the SOTERIA space weather research network between 16 centers on 11 EU countries (coordinator of the project), the NASA Sun Earth Connection Theory program and the NASA MMS-IDS project; a number of LANL internal projects and National Nuclear Security Administration (NNSA) projects; the Italian Institute for the Physics of Matter (INFM) project on non- neutral plasmas. Lapenta has published about 400 works (115 on international peer-reviewed journals).

Recent relevant publications ò X. Sun, G. Lapenta, L. Dorf, I. Furno, T. P. Intrator, Experimental onset threshold and magnetic pressure pile- up for 3D reconnection, Nature Physics , doi:10.1038/nphys1300, 2009. ò G. Lapenta, Self-Feeding Turbulent Magnetic Reconnection on Macroscopic Scales, Physical Review Letters , 100, 235001, 2008. ò G. Lapenta, D. Krauss-Varban, H. Karimabadi, J.D. Huba, L.I. Rudakov, P. Ricci, Kinetic Simulations of X- line Propagation in 3D Reconnection , Geophysical Research Letters , 33, L10102,doi:10.1029/2005GL025124, 2006. ò G. Lapenta, J.U. Brackbill, P. Ricci, Kinetic Approach to microscopic-macroscopic coupling in space and laboratory plasmas , Physics of Plasmas , 13, 055904, 2006. ò G. Lapenta, D.A. Knoll, Effect of a Converging Flow at the Streamer Cusp on the Genesis of the Slow Solar Wind , Astrophysical Journal , 624, 1049, 2005. ò G. Lapenta, J.U. Brackbill, Nonlinear Evolution of the Lower Hybrid Drift Instability: Current Sheet Thinning and Kinking , Physics of Plasmas , 9, 1544-1554, 2002. ò G. Lapenta, Simulation of Charging and Shielding of Dust Particles in Drifting Plasmas , Physics of Plasmas , 6, 1442-1447, 1999. ò G. Lapenta, J.U. Brackbill, A Kinetic Theory for the Drift-Kink Instability , Journal of Geophysical Research , 102, 27099-27108, 1997.

14 Li Bo School of Space Science and Physics Shandong University at Weihai, 264209, China Tel: +86-631-5673527 Fax: +86-631-5673638 email: [email protected]

Research Interests Bo Li 's research interests are with the roles of hydromagnetic waves in heating the solar corona and accelerating the solar wind. He combines multi-fluid models of the solar corona and solar wind with a forward modeling approach to infer what influences the beh avior of coronal plasma species in general, and those emitting Ultraviolet lines in particular.

Employment History Professor of Physics ( Supported by the Qilu Young Scholar 2009.06 – Program), Shandong University, China (Post-Doctoral) Research Assistant 2002.07 – 2009.03 Aberystwyth University, UK

Education Ph.D. in Space Physics 1996.09 – 2001.12 University of Science and Technology of China (USTC), Hefei, China 1992.09 – 1996.07 B.Sc. in Nuclear Physics, USTC, Hefei, C hina Selected Publications

O. W. Roberts, X. Li, & B. Li , Kinetic plasma turbulence in the fast solar wind measured by Cluster, Astrophysical Journal (ApJ), in press, (2013) B. Li , S. R. Habbal, & Y.-J. Chen, The period ratio for standing kink and sausage modes in solar structures with siphon flow. I. magnetized slabs, ApJ, doi:10.1088/0004-637X/767/1/1 (2013) B. Li , L.-D. Xia, & Y. Chen, Solar winds along curved magnetic field lines, Astronomy & Astrophysics (A&A), 529, A148 (2011) Y. Chen, S. Feng, B. Li , et al., A Coronal Seismological Study with Streamer Waves, ApJ, 728, 147 (2011) Bo Li , & Xing Li, Angular momentum transport in a multicomponent solar wind with differentially flowing, thermally anisotropic ions, A&A, 494(1), 361-371 (2009) Bo Li , & Xing Li, Effects of non-WKB Alfven waves on a multicomponent solar wind with differential ion flow, ApJ, 682(1), 667-678 (2008) Bo Li , & Xing Li, Propagation of non-Wentzel-Kramers-Brillouin Alfven waves in a multicomponent solar wind with differential ion flow, ApJ, 661(2), 1222-1233 (2007) Bo Li , Shadia Rifai Habbal, and Xing Li, Angular momentum transport and proton–alpha particle differential streaming in the solar wind, ApJ, 661(1), 593-601 (2007) X. Li, Q.-M. Lu, & B. Li , Ion pickup by finite amplitude parallel propagating Alfven waves, ApJ Letters, 661(1), L105-L108 (2007) B. Li , & X. Li, Effects of alpha particles on the angular momentum loss from the Sun, A&A, 456(1), 359-365 (2006) N. La brosse, X. Li, & B. Li , On the Lyman alpha and beta lines in solar coronal streamers, A&A, 455(2), 719-723 (2006) B. Li , X. Li, & N. Labrosse, A global 2.5-dimensional three fluid solar wind model with alpha particles, Journal of Geophysical Research(JGR), 111, A08106 (2006) S. T. Wu, B. Li , S. Wang, & Huinan Zheng, A three-dimensional analysis of global propagation of Magnetohydrodynamic (MHD) waves in a structured solar atmosphere, JGR, 110, A11102 (2005) Bo Li , X. Li, Y.-Q. Hu, & Shadia R. Habbal, A two-dimensional Alfven wave-driven solar wind model with proton temperature anisotropy, JGR, 109, A07103 (2004)

15

Riley Pete Predictive Science, Inc., 9990 Mesa Rim Road, San Diego, CA 92121, USA Tel: +1-858-217-5868 Fax: +1-858-408-1953 email: [email protected]

Experience Pete Riley has more than 16 years of experience studying the solar corona and inner heliosphere using a range of remote solar and in situ datasets as well as large numerical models. He is a team member of the STEREO, Ulysses, and ACE missions, and has published over 40 papers in the field of space physics, and particularly in the area of solar and heliospheric physics. He was and editor and Editor in Chief for Reviews of Geophysics, and was an associate editor for GRL. He regularly reviews papers for the JGR, GRL, APJ, MNRAS, and APJL, among others, and has been awarded an editors' citation for excellence in refereeing for JGR. He currently serves on a number of NASA and NSF panels/committees/definition teams, and is currently chair of NASA’s LWS Extreme Space Weather Events workshop steering committee. He also served as chair for NSF's SHINE steering committee. Pete is a member of the American Geophysical Union (AGU), the American Astronomical Society (AAS/SPD), and the International Astronomical Union (IAU). He has, and continues to receive PI funding from NASA, NSF, and DoD.

Education • Ph.D., Space Physics and Astronomy, Rice University, Houston, Texas, 1994. • M.Sc., Astronomy and Astrophysics, University of Sussex, Brighton, England, 1989. • B.Sc., Astrophysics, University College Cardiff, Cardiff, Wales, 1988.

Professional Activities • 2008 – Present Senior Research Scientist and Vice-President, Predictive Science. • 1999 – 2008 Research Scientist, Science Applications International Corporation. • 1996 – 1999 Post-Doc. and Technical Staff Member, Los Alamos National Laboratory • 1994 – 1996 Postdoctoral Fellow, Lunar and Planetary Lab, University of Arizona.

Related Recent Publications Riley, P., On the probability of occurrence of extreme solar events, Space Weather, 10, S02012, doi:10.1029/2011SW000734, 2012. Riley, P., et al., Corotating Interaction Regions during the Recent Solar Minimum: The Power and Limitations of Global MHD Modeling, JASTP, 83, 1-10, doi: 10.1016/j.jastp.2011.12.013, 2012. Riley, P. and J. G. Luhmann, Interplanetary Signatures of Unipolar Streamers and the Origin of the Slow Solar Wind, doi: 10.1007/s11207-011-9909-0, 2011. Riley, P., et al., On the relationship between coronal heating, magnetic flux, and the density of the solar wind, JGR, 115, A06104, doi:10.1029/2009JA015131, 2010. Riley, P., and D. J. McComas, Derivation of Fluid Conservation Relations to Infer Near-Sun Properties of Coronal Mass Ejections from in situ Measurements, JGR,114, 9102, 2009. Riley, P., R. Lionello, Z. Mikic, and J. A. Linker, Using Global Simulations to Relate the Three-part Structure of Coronal Mass Ejections to in situ Signatures, Ap. J., 672, 1221, 2008. Riley, P., Modeling corotating interaction regions: From the Sun to 1 AU, JASTP, 69, 32, 2007. Riley, P. et al., A Comparison between Global Solar Magnetohydrodynamic and Potential Field Source Surface Model Results, Ap. J., 653, 1510, 2006. Riley, P. and J. T. Gosling, On the origin of near-radial magnetic fields in the heliosphere: Numerical simulations, JGR, 112, A06115, doi:10.1029/2006JA012210, 2007. Riley, P. et al., A Comparison between Global Solar Magnetohydrodynamic and Potential Field Source Surface Model Results, Ap. J., 653, 1510, 2006. Riley, P. et al., On the rates of coronal mass ejections: remote solar and it in situ observations, Ap. J., 647, 648, 2006.

16 Strachan Leonard Harvard - Smithsonian Center for Astrophysics Cambridge, MA 02138, USA Tel: +1-617-496-7569 Fax: +1-617-495-7049 email: [email protected]

EDUCATION: Ph.D., Astronomy, 1990, Harvard University, Cambridge, Massachusetts, USA A.M., Astronomy, 1987, Harvard University, Cambridge, Massachusetts, USA S.B., Physics, 1982, Massachusetts Institute of Technology, Cambridge, Massachusetts, USA

PRIMARY RESEARCH INTERESTS: My research focuses on developing remote sensing techniques and instrumentation for studying the solar corona and solar wind using UV/EUV spectroscopy. Specifically, I am interested in determining the physical characteristics of the solar wind source regions of the solar corona. Such measurements are important for understanding the processes that drive both steady and dynamic solar wind. Previous experience includes participating in the instrument development and flight operations of the Spartan 201 space shuttle experiment.

RECENT POSITIONS HELD: 1991-Pres Astrophysicist, Smithsonian Astrophysical Observatory 1987-1991 Physicist, United States Air Force 1983-1987 Research Assistant, Harvard University

SELECTED PUBLICATIONS: L. Strachan, A.V. Panasyuk, & J.L. Kohl, “The evolution of plasma parameters on a coronal source surface at 2.3 Rs during solar minimum”, Ap J, 745, 51, 2012. L. Strachan, “Ultraviolet spectroscopic observations of coronal streamers in the SOHO era”, J. Astrophys. Astron., 29, 167, 2008. M. Uzzo, L. Strachan, & A. Vourlidas, “The physical properties of coronal streamers II” , Ap J, 671, 912, 2007. M. Uzzo, L. Strachan, A. Vourlidas, Y.-K. Ko, & J.C. Raymond, “Physical properties of a 2003 April Quiescent Streamer” , Ap J, 645, 720, 2006. L. Strachan, R., Suleiman, R., A.V. Panasyuk, D.A., Biesecker, & J.L. Kohl, “Empirical densities, kinetic temperatures, and outflow velocities in the equatorial streamer belt at solar minimum”, Ap J, 571, 1008, 2002. L. Strachan, A.V. Panasyuk, D. Dobrzycka, J.L. Kohl, G. Noci, S. Gibson, D.A. Biesecker, Y-K. Ko, and A.B. Galvin, “Latitudinal dependence of outflow velocities from O VI Doppler dimming observations during the SOHO Whole Sun Month”, JGR, 105, 2345, 2000. S.R. Cranmer, J. L. Kohl, G. Noci, E. Antonucci, G. Tondello, M. C. E. Huber, L. Strachan, et al., “An Empirical model of a polar coronal hole at solar minimum”, Ap. J., 511, 481, 1999. J. L. Kohl, G. Noci, E. Antonucci, G. Tondello, M.C.E. Huber, L.D. Gardner, P. Nicolosi, L. Strachan, et al., “First results from the SOHO Ultraviolet Coronagraph Spectrometer”, Solar Phys., 175,613, 1997. J. L. Kohl, L. Strachan, L. D. Gardner, “Measurement of hydrogen velocity distributions in the extended solar corona”, Ap. J. Let., 465, L141, 1996.

17 von Steiger Rudolf International Space Science Institute Hallerstrasse 6, 3012 Bern, Switzerland Tel: + 41-31-631-48-90 Fax: + 41-31-631-48-97 email: [email protected]

Degrees 1984 Lic. phil. nat. (diploma) in theoretical physics, Prof. P. Hajicek, Univ. of Bern 1988 Dr. phil. nat. (Ph.D.) in experimental physics, Prof. J. Geiss, Univ. of Bern 1995 Habilitation in “Experimentalphysik, insbesondere extraterrestrische Physik”, Phil.-nat. Faculty, Univ. of Bern

Positions 1988–1989 Research Associate, Physikalisches Institut, University of Bern 1990 Research Associate, Dept of Physics and Astronomy, Univ. of Maryland, College Park 1991–1995 Research Associate, Physikalisches Institut, University of Bern 1995–1999 Senior Scientist, International Space Science Institute (ISSI) in Bern 1998 Visiting Research Scientist, University of Michigan, Ann Arbor (4 months) since 1999– Director, International Space Science Institute (ISSI), Bern, and Associate Professor (Extraordinarius), University of Bern

Projects • Theoretical modelling of the First Ionisation Potential (FIP) fractionation effect in the solar atmosphere • Charge Energy Mass (CHEM) sensor on AMPTE/CCE • Solar Wind Ion Composition Spectrometer (SWICS) on Ulysses, CoI since 1991 • Solar Wind Ion Composition Spectrometer (SWICS) on ACE

Awards • Swiss National Science Foundation: Young Researcher Award (1990) • Several Group Achievement Awards from ESA and NASA • International Academy of Astronautics (IAA): Full member

Professional Services • Mercury Orbiter (now BepiColombo), member of the Assessment Study Group (1993-94) • Committee on Space Research (COSPAR): Chair of Commission D (2004- ) • Space Science Reviews: Editorial Committee member (2005- ) • NASA HGIP Panel member (2007) • Evaluator for EC FP7-SPACE.2012-1 call (2012, 2013) • Member of Geophysical and Astronomical Societies: EGU, AGU, IAU, AAS, SGAA • Referee for ApJ, GRL, JGR, SSRv, and other professional journals

Extracurricular • Member, Council and Finance Commission, Burgergemeinde Bern • Obmann (President), Gesellschaft zu Ober-Gerwern, Bern • Member, “HUGO in the sky”: Project approaching science data with electronic sounds and improvised music

Selected Publications (from about 100 in refereed journals) - R.von Steiger and T. H. Zurbuchen, “Polar coronal holes during the past solar cycle: Ulysses observations”, J. Geophys. Res., 116, A01105, 2011 - R. von Steiger, T. H. Zurbuchen, and D. J. McComas, “Oxygen flux in the solar wind: Ulysses observations”, Geophys. Res. Lett., 37, L22101, 2010. - R. von Steiger, The solar wind through the solar cycle, in A. Balogh, L. J. Lanzerotti, and S. T. Suess (eds.), “The Heliosphere through the Solar Activity Cycle”, London: Springer Praxis Publishing, 41–78, 2008. - R. von Steiger, N. A. Schwadron, J. Geiss, G. Gloeckler, L. A. Fisk, S. Hefti, B. Wilken, R. F. Wimmer- Schweingruber, and T. H. Zurbuchen, “Composition of quasi-stationary solar wind flows from SWICS/Ulysses”, J. Geophys. Res., 105, 27,217–27,238, 2000.

18 Wang Yi-Ming Space Science Division, Naval Research Laboratory Washington, DC 20375-5352, USA Tel: +1-202-404-8460 Fax: +1-202-404-7997 email: [email protected]

Present Position: Astrophysicist, Naval Research Laboratory

Education: Harvard College (AB, Astronomy, 1971) MIT (ScD, Physics, 1976)

Employment: Astronomy Centre, University of Sussex (1976-1979) Astronomische Instit ute der Universit
at Bonn (1979-1986) Space Science Division, Naval Research Laboratory (1986-present)

Related Activities: Associate editor, JGR - Space Physics (2001-2004)

Professional Societies: AAS, AGU, IAU

Awards : 2011 NRL Sigma Xi Award for Pure Physics

Refereed Journal Publications: 160

RECENT PUBLICATIONS ON SLOW SOLAR WIND

• “Slow solar wind from open regions with strong low-coronal heating", Wang, Y.-M., Ko, Y.-K., & Grappin, R., Astrophys. J., 691, 760 (2009) • “The structure of streamer blobs", Sheeley, N. R., Jr., Lee, D. D.-H., Casto, K. P., Wang, Y.-M., & Rich, N. B., Astrophys. J., 694, 1471 (2009) • “Time-dependent hydrodynamical simulations of slow solar wind, coronal inows, and polar plumes", Pinto, R., Grappin, R., Wang, Y.-M., & L_eorat, J., Astron. Astrophys., 497, 537 (2009) • “Formation and evolution of coronal holes following the emergence of active regions", Wang, Y.-M., Robbrecht, E., A. P. Rouillard, Sheeley, N. R., Jr., & Thernisien, A. F. R., Astrophys. J., 715, 39 (2010) • “On the relative constancy of the solar wind mass ux at 1 AU," Wang, Y.-M., Astrophys. J., 715, L121 (2010) • “Semiempirical models of the slow and fast solar wind," Wang, Y.-M., Space Sci. Rev., 172, 123 (2012) • “On the nature of the solar wind from coronal pseudostreamers", Wang, Y.-M., Grappin, R., Robbrecht, E., & Sheeley, N. R., Jr., Astrophys. J., 749, 182 (2012) • “The solar wind and interplanetary field during very low amplitude sunspot cycles," Wang, Y.- M., & Sheeley, N. R., Jr., Astrophys. J., 764, 90 (2013)

19 Appendix C

References of the project

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