PI: Vladimir Slemzin, LPI, Moscow Co-I: Sergey Kuzin, Alexander Urnov, Farid Goryaev - LPI

Study of the solar inner corona and search for coronal streams from active regions using SWAP

off-disk observations

PI: Vladimir Slemzin, LPI, MoscowCo-I: Sergey Kuzin, Alexander Urnov, Farid Goryaev - LPI Louise Harra – MSSL/UCL

Proposal to the PROBA 2 Guest Investigator Program. June 1, 2010

SPIRIT studies of the inner corona (Slemzin et al., AnGeo 2008)


R=1.1

Helmet-like structure

Overlay of the disk and corona images

Stray lightStray lightIn the Hershel telescopes the level of straylight is lower than in the Ritchey-Chretien In the Hershel telescopes the level of straylight is lower than in the Ritchey-Chretien telescopes telescopes (large mirror- detector distance, no elements in between)(large mirror- detector distance, no elements in between)PSF is measured during eclipsesPSF is measured during eclipses

304 A 175 A2002-06-11 01:06:40 5

Radial distribution at the equatorial plane

Ts =1.53 MK

1.62 MK

1.32 MK

Hydrostatic approach: radial distribution of radiation in EUV emission lines excited by collisions (I ~ Ne

2)

sun

ss

sssun

RmgkTH

rrHrrTrErHRrI

0

0

00

2/3 )(2exp),()(

- density scale of height

Ts – hydrostatic temperature

12

Quiet sun04/04/96

Active sun16/06/02

Sources of the solar windQuasi-stationary solar wind

at 1 AU

fast SW (600-800 km/s)

slow SW (400-600 km/s)

Quasi-stationary coronal streams (from several days to several rotations)

Streams from polar coronal holes, polar rays and plumes

WL streamers

Streams from ARs, low-latitude CHs

Transient solar wind (200-700 km/s)

Transient streams (several hours) CME Jets small-scale events

Main task and goals of the proposal Main task: to study the global and local structure of the

solar inner corona from the limb to ~ 2 Rsun by means of the SWAP off-disk EUV observations in coordination with Hinode/EIS.

Goals: • Global survey of the inner corona at rising solar activity

and comparison of its structure with measurements at solar maximum (SPIRIT) and deep minimum (TESIS).

• Search of the solar wind streams from active regions.

• Determination of physical properties of the coronal streams and other local magneto-plasma formations.

Association of the solar wind streams with solar sources

1).Temporal correlation between the solar wind variations and the solar rotation

2). Outflows from solar sources detected by the Doppler shift of coronal lines

3). Tracing of the coronal rays from the solar source to the outer corona (streamer)

4). Ionic composition of the plasma in the solar source and at 1 AU

FIP bias (enhanced FIP abundances)Fe/O ratio O+7/ O+6 ratio (freeze-in temperature)

SWAP data

1x10s 100x10s equatorial scan


100x10s


N W S E N

1x10s


SWAP – LASCO C2

Global view of the inner corona combined from 4 SWAP off-point images (±10’)

LASCO C2 FOV LED

Doppler velocity

Intensity

Outflows of up to 50 km/s are seen in the boundary of AR, Harra et al. (2008).


Detection of coronal outflows with Hinode/EIS

Hinode/EIS data

• Two EUV bands: 170-210 Å and 250-290 Å• CCD camera; Two 2048 x 1024 high QE back illuminated CCDs• Spatial resolution: 1 arc sec pixels/2 arc sec resolution• Line spectroscopy:• ~ 25 km/s per pixel sampling• ± 3 km/s with ~ 200 counts in a line profile• Field of View:

– Raster: 6 arc min × 8.5 arc min (max height: 17 arc min)– FOV centre moveable E – W by ± 15 arc min

• Wide temperature coverage: log T = 4.9, 5.3, 5.4, 5.8, 6.0 - 7.3 K• 4 slit/slots – 1”, 2”, 40”, 266”


TESIS – EIS comparison1 August 2009 8 August 2009


TESIS Fe IX-X 171 AAR near small CH


TESIS 1-8 August 2009

Hinode/XRT TESIS 01/08/2010 18:05 UT 01/08/2010 11:26 UT



TESIS FeIX-X 171 A EIS FeXII 195 A intensity


TESIS FeIX-X 171 A EIS FeXII 195 A Doppler velocity

outflow


TESIS – LASCO C2

CH

CH

AR

Solar wind data - ACE

Working plan of the research1). Study of the quiet corona by full global survey of the inner corona

up to 2 Rsun in 4 off-limb positions. Comparison with the TESIS and SPIRIT data

2). Search of coronal streams originated from active regions (SWAP in coordination with Hinode/EIS):- Search of the coronal outflows in the active regions near the center of the disk and selection the target object (EIS). - Observation of the targeted AR during a week (SWAP in standard mode, 10s/1 min);- Search of the coronal rays from the targeted AR at the limb (SWAP in the W- off-disk mode, 100x10s series, during 2-3 days). The ray should be identified as a bright line having a counterpart in the WL streamer.

3). Diagnostics of plasma in the limb region of the coronal rays and nearby in the corona by the DEM method (using the EIS data in the off-limb mode):Te, Ne, FIP bias


Timeline of observations22/06 SWAP global view (4 pos*100 frames) - Rot.019/07 SWAP global view (4 pos*100 frames) - Rot.111/08 SWAP solar eclipse15/08 SWAP global view (4 pos*100 frames) - Rot.212/09 SWAP global view (4 pos*100 frames) - Rot.3

T0 EIS start of monitoring ARs at the disk

T1 EIS outflow detection -> warning to SWAPT1+6d SWAP two-days off-point monitoring (W-limb) position of rays –>

warning to EISEIS monitoring the ray and nearby regions at the limb

Plan of visits and presentations5-19/11 2010 visit to ROB processing of the data, preparation

of LPI – 2, MSSL-1 the report on structure of the global 15 days inner corona to ESWW 2010

(Brugge, 15-19/11 2010)

20/03 – 2/04 2011 visit to ROB processing of the data, preparation of LPI – 1, MSSL-1 the report of preliminary results to EGU 15 days 2011 (Vienna, 3-8 April 2011).

PI: Vladimir Slemzin, LPI, Moscow Co-I: Sergey Kuzin, Alexander Urnov, Farid Goryaev - LPI

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