Proposal to the PROBA 2 Guest Investigator Program. June 1, 2010
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PI: Vladimir Slemzin, LPI, Moscow Co-I: Sergey Kuzin, Alexander Urnov, Farid Goryaev - LPI PowerPoint PPT Presentation


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Proposal to the PROBA 2 Guest Investigator Program. June 1, 2010. Study of the solar inner corona and search for coronal streams from active regions using SWAP off-disk observations. PI: Vladimir Slemzin, LPI, Moscow Co-I: Sergey Kuzin, Alexander Urnov, Farid Goryaev - LPI

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

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

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

PI:Vladimir Slemzin, LPI, Moscow

Co-I:Sergey Kuzin, Alexander Urnov, Farid Goryaev - LPI

Louise Harra – MSSL/UCL


R=1.1

Helmet-like structure

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

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


Overlay of the disk and corona images

Stray light

In the Hershel telescopes the level of straylight is lower than in the Ritchey-Chretien telescopes (large mirror- detector distance, no elements in between)

PSF is measured during eclipses

304 A 175 A

5

2002-06-1101:06:40


Radial distribution at the equatorial plane

Ts =1.53 MK

1.62 MK

1.32 MK

Active sun

16/06/02

Quiet sun

04/04/96

Hydrostatic approach: radial distribution of radiation in EUV emission lines excited by collisions (I ~ Ne 2)

-density scale of height

Ts– hydrostatic temperature

12


Sources of the solar wind

Quasi-stationary solar wind at 1 AU

fast SW (600-800 km/s)

slow SW (400-600 km/s)

Quasi-stationarycoronal 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)


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

SWAP data

1x10s 100x10s equatorial scan


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

1x10s

N W S E N

100x10s


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

SWAP – LASCO C2


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

LASCO C2 FOV LED


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

Detection of coronal outflows with Hinode/EIS

Doppler

velocity

Intensity

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


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

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”


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

TESIS – EIS comparison

1 August 20098 August 2009

AR near small CH

TESIS Fe IX-X 171 A


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

TESIS 1-8 August 2009


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

Hinode/XRTTESIS 01/08/2010 18:05 UT 01/08/2010 11:26 UT


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

TESIS FeIX-X 171 A EIS FeXII 195 A intensity


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

outflow

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


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


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


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

TESIS – LASCO C2


Solar wind data - ACE

AR

CH

CH


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

Working plan of the research

1). 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 observations

22/06 SWAPglobal view (4 pos*100 frames) - Rot.0

19/07 SWAPglobal view (4 pos*100 frames) - Rot.1

11/08SWAPsolar eclipse

15/08 SWAPglobal view (4 pos*100 frames) - Rot.2

12/09 SWAPglobal view (4 pos*100 frames) - Rot.3

T0 EISstart of monitoring ARs at the disk

T1EISoutflow detection -> warning to SWAP

T1+6d SWAPtwo-days off-point monitoring (W-limb) position of rays –> warning to EIS

EISmonitoring the ray and nearby regions at the limb


Plan of visits and presentations

5-19/11 2010visit to ROB processing of the data, preparation ofLPI – 2, MSSL-1the report on structure of the global 15 daysinner corona to ESWW 2010

(Brugge, 15-19/11 2010) 

20/03 – 2/04 2011 visit to ROBprocessing of the data, preparation of LPI – 1, MSSL-1 the report of preliminary results to EGU 15 days2011 (Vienna, 3-8 April 2011).


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