Initial Results of Mingantu Ultrawide SpectralRadioheliograph--- the Chinese Spectral RadioheliographYihua Yan
Key Laboratory of Solar Activity
National Astronomical Observatories, Chinese Academy of Sciences
Beijing 100012, China

With CSRH Team including: Z Chen, W Wang, F. Liu, L. Geng & J Zhang**Peking University, Beijing, China
National Major Scientific Research Facility R&D Program （ZDYZ2009-3）
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3rd AOSWA Workshop, Fukuoka, Japan

Outline• Radio imaging-spectroscopy• Construction of CSRH
• Initial Observations• Summary

2015.3.3

3rd AOSWA Workshop, Fukuoka, JapanScientific Motivations:• Radio bursts are prompt indicators of the various
solar activities including flares and CMEs, etc.

（Benz 2009）2015.3.3

3rd AOSWA Workshop, Fukuoka, Japan

Scientific Motivations:• The available radio facilities are either with hightime and spectral resolution but without spatial
resolution, or with high time and spatial resolution
but at only one or a few frequencies.
• It is needed to have high spectral resolution overwide band as well (Gary 2013).
• Imaging spectroscopy over cm-λ & dm-λ isimportant for addressing the problems of primaryenergy release, particle acceleration, andtransportation processes, and the coronal magnetic
fields (Bastian, et al., ARAA, 1998; Gary & Keller 2004;
Aschwanden 2004; Pick & Vilmer 2008, Klein et al. 2008;
Tomczyk et al. 2013).
• MWA, LOFAR, etc., at metric and lower frequencies,and ALMA at mm, THz.
2015.3.3

3rd AOSWA Workshop, Fukuoka, Japan→ require a new instrument:

capable of true imaging
spectroscopy, with hightemporal, spatial, and spectral
resolution ---- CSRH orFASR(Hudson & Vilmer 2007, Pick &Vilmer 2008, Klein et al 2008, Tomczyk,et al 2013).

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3rd AOSWA Workshop, Fukuoka, Japan

CSRH Specifications(Yan et al. 2009 Earth, Moon Planet; 2013 IAUS 294; Wang et al.
2013 PASJ)

Range
Frequency Res.

~0.4–15 GHz （λ：~75 –2 cm）
64
chan (I: 0.4-2 GHz)
>32 (520) chan (II: 2-15 GHz)
Spatial Res.
1.3”– 50”
Temporal Res.
I: ~ 25 ms
II: ~200 ms
Dynamic Range
25 db （snapshot）
Polarizations
Dual circular L, R
Array
I: 40×4.5m
II: 60×2m parabolic antennas
Lmax
3 km
Field of view
0.6°– 7°2015.3.3

3rd AOSWA Workshop, Fukuoka, JapanCSRH-I 40-antenna Array & UV
Coverage at 1 GHz

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CSRH-II 60-antenna Array & UVCoverage at 10 GHz

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Site and Construction of CSRH

Inner Mongolia, China

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Site survey~400kmNokia Map

3rd AOSWA Workshop, Fukuoka, Japan

Array Construction

Ming’antu Observing Station Plan
July 2014
Aug2012

Plan of Mingantu
Observing
Station in 2014
Approvedand start
construction

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3rd AOSWA Workshop, Fukuoka, Japan

CSRH-I in CASA

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3rd AOSWA Workshop, Fukuoka, Japan

FY-2 satellite 1.7 GHz (CSRH Beam at 1.7GHz)
Dynamic Range in cleaned map： about 30dBDirty Beam2015.3.3

Cleaned Beam

3rd AOSWA Workshop, Fukuoka, Japan

Test observations with CSRH-I

Test of Cyg A observed at 1.7
GMRT 610 MHz Image
GHz on 5 Jun 2013 at 5:30 UT（not scaled, GMRT web）
with 1s integral time.
(Signals 2 orders weaker than that of the Sun!)2015.3.3

3rd AOSWA Workshop, Fukuoka, Japan

Preliminary result with 30 ms integral time

CSRH-I image of thequiet Sun at 1.7GHzand comparisons withother observations on
22 Jan 20142015.3.3

3rd AOSWA Workshop, Fukuoka, Japan

Preliminary result with 30 ms integral time

CSRH-I
image of thequiet Sun at
1.7GHz andcomparisonswith SDO
EUV 171A
image andmagnetogramon 12 May
2014 at05:15UT
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3rd AOSWA Workshop, Fukuoka, JapanA solar flare and radio bursts on 11 Nov, 2014

NoRP

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The solar flare starting at 04:22 on 11 Nov 2014

GOES SXRAIA131 movie
SGD associates the radio burst withthe disk center flare event
AIA 1712015.3.3

3rd AOSWA Workshop, Fukuoka, Japan

HMI / SDO

The source of radio bursts starting at 04:22:20UTlocated at east limb (Preliminary results)

2015.3.3

3rd AOSWA Workshop, Fukuoka, Japan• Left-circular & Right-circular polarizations (Preliminary results)• 04:23-04:24UT@5s interval & 3ms integral time

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SDO／AIA
94、131、171、304A
movie

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SDO/AIA observations indicate aneruptive process

2015.3.3

3rd AOSWA Workshop, Fukuoka, JapanLASCO／C2 &Wind radio bursts

2015-1-13

太阳活动重点实验室2014年学术年会，怀柔2015.3.3

3rd AOSWA Workshop, Fukuoka, Japan

Positions of STEREO A and B for2014-11-11 04:20 UT

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Radio sources & STEREO image(Preliminary results)
LASCO/C2 CME

Radio source movement

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3rd AOSWA Workshop, Fukuoka, Japan

CSRH-II Preliminary Results of ASIA-7 satellite at 12 GHz
on 15 Aug, 2014Beam2015.3.3

3rd AOSWA Workshop, Fukuoka, Japan

Phase closure ~<1° (RMS) for satellite signalof 700 min in the night of 4-5 Feb 2015 for all
baselines until 3 km of CSRH-II(N.B. Specification Phase closure <7° should be OK)
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3rd AOSWA Workshop, Fukuoka, JapanAR2129：Largest sunspot, energetic X-classtwo-ribbon flares, no CMEs (Hudson，2014)
Net flux～2%
whereas ～25% flux imbalancefor δ-spot（Wang&Shi，1994）

http://sprg.ssl.berkeley.edu/~tohban/wiki/
index.php/RHESSI_Science_Nuggets
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CSRH-IIBurst on 22Oct-2014
2G0511 0517 peak M2.7

8.5G

15G05:10:14UT
2015.3.3＃2192

Radio bursts
confined in highfrequency band,
agreeable withthe scenario: low
altitude activity,no CME

05:20:14UT

3rd AOSWA Workshop, Fukuoka, Japan

Another burst event on Dec 17 2014 for a M8.7 flare2015.3.3

3rd AOSWA Workshop, Fukuoka, Japan

CSRH-I radio burst fine structures,
imaging processing being underway

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Station Construction Starting
EU FP7 RadioSun 1stWorkshop, 30 Oct 20132015.3.3

3rd AOSWA Workshop, Fukuoka, Japan

SummaryI.

II.

Solar radio imaging spectroscopy is in its
infancy and will open new observational
windows on flares and CMEs. It will also provide
coronal magnetograms. Complementary to Xray, γ-ray, UV/EUV etc. observations.
For CSRH, radio quiet zone protection of 10km
radius is established. CSRH-I & II have been
constructed and renamed as M USER :– Calibration and verification– Commissioning observations– Put into operation in middle 2015

III. Develop data pipe-line
IV. Observing Station construction in 2015
V. MUSER Initial observations are promising2015.3.3

3rd AOSWA Workshop, Fukuoka, Japan(Photo by S.J. Yu)
2015.3.3

3rd AOSWA Workshop, Fukuoka, Japan