Overview of White Light & Radio Signatures of CMEs Angelos Vourlidas Naval Research Laboratory.

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Presentation transcript:

Overview of White Light & Radio Signatures of CMEs Angelos Vourlidas Naval Research Laboratory

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 2 Lecture Outline Related Lectures: –Overview: Space weather –CME/SEP Obs & Models: SEPs, Coronal/IP Shocks –Basic Physics: Reconnection, radio seminars –Practicum: In-situ measurements, Radio instrumentation Outline: –Overview of radio & white light (WL) emissions –Highlights of joint WL & radio observations of CMEs –Open questions/research topics –Review

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 3 Why treat radio & WL together? Both emissions are due to coronal electrons –THERMAL radio emission goes as N e 2 dl –WL emission goes as N e dl Both emissions are insensitive to the temperature of the plasma Both are probes of the extended corona & heliosphere Radio observations are possible on the disk (no occulter) AND trace CMEs (indirectly) all the way to the Earth

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 4 Review of White Light Emission A feature can be bright because: –It is extended ALONG the line of sight (many electrons) –It has mass (many electrons) –It is close to the plane of max. scattering A feature disappears because: –It was carried away (in a CME) –It was pushed AWAY from plane of max. scattering Front Core Cavity Streamers Occulter Pylon

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 5 Review of Radio Emission Emission Mechanisms Thermal Non-Thermal Chromosphere (GHz) Aurora (KHz) Range of Observations Types of radio data time frequency AIP Spectrum SSRT 5.7 GHz Image

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 6 Review of Radio Bursts Type III: relativistic electrons (.3c) Type II: shock-related (~1000 km/s) Type IV: post-CME reconfiguration From Wild et al (1963)

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 7 How we use WL & radio observations? We will review how the joint analysis of coronagraph and radio data can lead to insights in the following: CME Initiation Structure of CMEs Early CME evolution Physical properties of CMEs CME shocks, accelerated particles CME propagation

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 8 What about CME Precursors? WL: Rising and expanding streamer ( when cadence allows ) for hours ( days in streamer-blowouts ) before the CME erupts

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 9 Drifting continuum sources may mark the CME birth. Radio Precursors of CMEs More work is needed to establish reliable radio precursors for CMES. The role of Noise Storms remains controversial.Noise Storms Some noise storm changes correlate with CME. Noise storm sometimes starts before CME and sometimes after.

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 10 CMEs are not ‘puffs of coronal smoke’ WL: CMEs contain large structures (e.g., filaments)

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 11 Follow Eruptive Filaments. Radio imaging of CME features Follow the initial activation with high cadence. Trace the coronal structures that participate in the eruption. NoRH (17GHz) NRH (410 MHz)

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 12 Does the CME evolve before appearing in the coronagraph? WL: Observe CME evolution only above ~2 R WL: Often CME expands over the whole disk

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 13 Kanzelhohe Hα images NRH sources at 236 MHz Artemis IV spectrum EIT dimming Radio Imaging of on-disk CMEs

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 14 Full CME expansion < 10 min. Indications of long range interactions. Erupted systems can be identified. Trace the CME initiation and development in the low corona. Limb Radio Imaging of Limb CMEs

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 15 CMEs are magnetic entities WL: CMEs contain magnetic structures (filaments) WL: Propagate as coherent systems In-situ: observations are fitted with fluxrope models

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 16 Image directly radio CME loops for the first time. Physical Properties of CMEs

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 17 Physical Properties of CMEs Image fine-scale CME structures. Derive physical parameters: B CME ~0.1-few G, E ~ 0.5-5MeV, n th ~10 7 cm -3

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 18 CMEs can drive shocks & accelerate particles WL: CME-driven shocks are a long-sought feature. Likely visible in many LASCO CMEs. WL: Accelerated particles cause “snow storms” on LASCO CCDs.

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 19 Radio CME front is faint. Several candidates for Type-II emission can be identified. Identify the shock at the CME front. Radio imaging of CME shocks

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 20 Type-II bursts remain unreliable proxies of solar eruptions Type-II Emissions and CMEs A technique for Type-II / LASCO analysis. Consistency between LASCO densities and Type-II profiles can pinpoint the CME: launch time, position angle and type-II source region 90% of EUV waves are associated with metric Type-IIs But EUV waves are better correlated to CMEs Type-IIs are blast waves (30%), CME-driven (30%) or behind CME (30%)

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 21 CMEs can interact with each other

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 22 Radio signs of CME interaction

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 23 CMEs evolution in the heliosphere? WL: Observational gap between 30 R (C3 FOV) and 80 R (inner edge of SMEI). Models: CMEs over-expand out of the ecliptic and compress radially Odstrcil et al (2003)

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 24 A Fast Limb CME: 31 May 2003 LASCO C3; 31, 04:18

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 25 IPS Mapping of CMEs. Radio mapping of ICMEs Follow the CME evolution in IP space. ORT (327MHz)

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 26 Continuous Spectral Coverage of Radio Solar Emissions. ICME tracking with radio spectra Establish the flare/CME/Type-II temporal relation. Multiple Type-II sources. Evidence for shock-accelerated electrons.

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 27 Contributions of radio/WL observations CMEs evolve/form rapidly in the low corona (~<15 mins). The features seen in WL could originate from a large area of the corona (front & back). CMEs are magnetic, large-scale structures. Electrons are accelerated in the low corona throughout the event. CMEs may interact with each other.

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 28 Open Questions What do the radio signatures tell us about the initiation mechanism? Where to the accelerated particles originate (flare or CME shock)? Can we find a reliable CME precursor in the radio? What can we learn about the CME evolution in the heliosphere from radio? Can we probe the magnetic structure of a CME with radio? Can we detect the thermal emission from CMEs?

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 29 Advantages of radio observations for CME studies Accurate timing of eruption initiation and development. Derivation of physical parameters in the eruptive structures (when thermal). Positional information on Type-II (shocks) sources. Identification of electron acceleration sites. Tracking the CME evolution from birth to Earth. Discovery of precursors to solar eruptions.

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 30 Backup Slides

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 31 Summary Shortcomings of Radio Observations: –Inadequate imaging (few frequencies, hours, low sensitivity). –Wide variation in the spectrometer characteristics (coverage, sensitivity). –Physics of Type-II emission are poorly understood. Solution Broadband imaging spectroscopy from a solar-dedicated instrument:

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 32 Detections of shocks in other regimes. Radio Type-II Emissions & CMEs Radio signatures of CME interactions. Radio signatures of CME interaction at large distances (Gopalswamy et al. 2001; Reiner et al. 2002). UVCS detection of a shock (Raymond et al. 2000). Yohkoh/SXT detection of a shock (Khan & Aurass 2002). Detection of a 17 GHz signature of an EUV wave (Aurass et al. 2002; White et al. 2002). VLA observes at 75 MHz. Bursts seen around CME times suggest long-term particle acceleration (Willson et al. 1998; Willson 2000). No detection of thermal CME emission (Gary et al. 2003).

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 33 “Type-II”-like sources in white-light images WIND AIP NRH ? ? 10:02 UT ( extrapolated )

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 34 Noise Storms

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 35 May 2, 1998 Radio CME 10 min of the radio CME

2 nd SPD Summer SchoolWhite Light & Radio CME Observations --- A. Vourlidas 36 What’s New in Cycle 23 LASCO/EIT revolutionize the study of solar eruptions. Nançay radioheliograph acquires imaging capability. WAVES records radio bursts in the unexplored region <15 MHz. AIP, Culgoora, BIRS, Artemis and several other spectrographs are operational (none in US). VLA acquires 75 MHz capability. Nobeyama Radioheliograph analysis focuses on eruptions. Gauribidanur Radioheliograph is operational. Ooty telescope produces IPS maps of CMEs. GMRT has solar observing capability. Siberian Solar Radio Telescope observes in 5.7 GHz. Huairou spectrograph data become available. Solar Radio Burst Locator will come online soon.