Solar flare studies with the LYRA - instrument onboard PROBA2
New ground based instrument initiatives for solar and...
Transcript of New ground based instrument initiatives for solar and...
New ground based instrument initiatives for solar and solar terrestrial physics
Alexei A. Pevtsov (National Solar Observatory, USA)
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New ground based instrument initiatives for solar and solar terrestrial physics
Alexei A. Pevtsov (National Solar Observatory, USA)
Information about projects was provided by:
Dale Gary (NJIT, USA) Gregory Fleishman (NJIT, USA) Hui Li (Purple Mountain Observatory, China)Andrey Tlatov (Kislovodsk Mountain Astronomical Station, Russia)Mikhail Demidov (Institute for Solar-Terrestrial Physics, Russia)Yihua Yan (National Astronomical Observatories, China)Zhong Liu (Fuxian Solar Observatory, China),Thomas Rimmele (National Solar Observatory, USA)Mei Zhang (National Astronomical Observatories, China)Robertus von Fay-Siebenburgen (U.K. and Hungary)Markus Roth (KIS, Germany)
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Summary of new instrument developments• Long-term synoptic networks (full disk, multi-wavelength, magnetic
field, imaging and helioseismology)• Coronal magnetic fields (radio, He10830)• Super high-resolution (large aperture) instruments• Sun-as-a-star instruments, Brazilian magnetograph project, existing
facilities etc.
Full disk and synopticmagnetograms
Imaging data High resolution Off-limb/on disk coronal magnetic field
Future Synoptic Networks• EU: SPRING network (future replacement for GONG): 4-6 sites,
0.5-m telescopes, SOLIS-type mount, multi-wavelength helioseismology and vector magnetography (Solarnet during the EU FP7).
• US: GONG refurbishing and upgrade (October 1, 1995, 2001 –GONG++)
• Japan: CHAIN - Continuous Hα Imaging Network• Russia: restoration of “Solar Service” Program (1932-1998, 16
stations); STOP network; network of small telescopes• Hungary: SOMNET (Solar Activity MOF Monitor)• Greece: Ionospheric and solar SW facility (Hα + ionospheric
TEC using DIGISONDE station).
FP7 Horizon 2020
Continuous Hα Imaging Network (CHAIN)Japan
https://www.kwasan.kyoto-u.ac.jp/CHAIN/
1992
2010
2017
+ Algeria?
Lat. 52N Long 104E deg.Lat. 44N Long 42E deg.
Russia
Polar fields
HMI/SDO WSO
SOLISKislovodsk
Network of automatic telescopes/spectro-heliographs for universities for observing in Hαand Ca II K.
Russia
DopplergramsMagnetograms
Synoptic solar telescope based on Magneto Optical Filter (MOF) technology: SAMM
MOF technology
2 observation lines at 2 altitudes in the solar atmosphere:
Na D2 (600-700 km)K I (300-400 km)
Future: Ca I (1000 km), He 1083Synoptic
Fixed wavelength but high stability and sensitivity
Full-disk or near-full-disk monitoring of solar activity
Hungary
SAMM: Realisation – Gyula SO
Hungarian Solar Physics Foundationwww.hspf.eu
Future SAMNet:
Photo-/Chromosphere/Coronal Magnetic Field
• The Daniel K Inouye Solar Telescope (DKIST) – 4m• He I 10830 magnetic field measurements (DST/Sac Peak) • SOLIS – 0.50m (relocated to BBSO)• SOLar SYnoptic Telescope (SOLSYT) – 0.35m
Russia
Coronal magnetic field (He10830, radio)
• HAO’s the COronal Solar Magnetism Observatory (COSMO,https://www2.hao.ucar.edu/cosmo) – 1.5m
• The Coronal Magnetism Telescopes of China (COMTEC) – 1.5m (Full Stokes profiles in three coronal forbidden lines (5303Å, 10747Å & 10798Å) and two chromospheric lines (5876Å & 10830Å); ~ 1 Gauss precision and 5" spatial resolution in about 10 minute cadence
• Full Stokes Polarimetry in He10830 (GREGOR, Dunn Solar Telescope)• Expanded Owens Valley Solar Array (EOVA), A 13-antenna interferometer
array operating over frequency range 1-18 GHz. Provides dynamic (1 s) “imaging spectroscopy” (at more than100 frequencies)
• Mingantu Spectral Radioheliograph (MUSER)
Freq range: 0.4-15 GHzFreq resolution:
64 chan(0.4-2.0GHz)~500 chan(2.0-15GHz)
Spatial resolution: 1.3˝-50 ˝ Time resolution: ~100 msMax. baseline: 3.0 km
MUSER-I MUSER-II
40-antenna Array
60-antenna Array
Mingantu Spectral Radioheliograph (MUSER)
Station Construction Progress (May 2015 – Present)
Solar Flares (e.g. 2017-Sep-10 X8.2)
SCOSTEP Toronto Gary et al. (2018), ApJ, submitted
EOVSA radio emission for this flare is distributed in three locations:1. Above bright EUV loops2. At sources flanking both sides,
associated with a larger loop that may be the legs of a CME
3. Along the plasma sheet connecting the rising cavity with the bright EUV loops.
The multi-frequency images form a data cube that provides spatially-resolved microwave spectra at each point in the source, which can be fit with multi-parameter theoretical spectra to provide B field and other parameters.
Fitting of Evolving Imaging Spectroscopy Data• Key 1: use of physically meaningful objective function
(GS + free-free)• Key 2: fast algorithms and codes
Derived parameter maps and accuracy evaluation
Unfolded Folded Unfolded Folded
Unfolded Folded Unfolded Folded
High-resolution ground based instruments
• McMath Pierce telescope – 1.7m• Goode Solar Telescope (GST) – 1.6m (bbso.njit.edu/)• GREGOR Solar Telescope – 1.5m (www.leibniz-kis.de/en/observatories/gregor/)• Swedish Solar Telescope (SST) – 1m
(www.isf.astro.su.se/)• New Vacuum Solar Telescope (NVST) – 1m (fso.ynao.ac.cn)• Dutch Open Telescope (DOT) – 0.45m (mothballed)
Large Aperture ground based instruments
• The Daniel K Inouye Solar Telescope (DKIST) – 4m (dkist.nso.edu)• The European Solar Telescope (EST) – 4m (www.est-east.eu)• Chinese Giant Solar Telescope (CGST) – 5m/8m
22m2 (5m) collecting area & 8m resolution diameter
1. High resolution observations of solar atmosphere(Photosphere & Chromosphere)2. High-accuracy measurement of Solar magnetic field(Photosphere & also Chromosphere)
0.03 arc-second @1.0 microns ( ~20km )0.04 arc-second @1.5 microns ( ~30km )
The Daniel K Inouye Solar Telescope
http://dkist.nso.edu/8 years of construction; 80% complete
D =SNR
0.7N10−0.4mo τΔλQφ2px texp
SNR ≈104
φpx ≈ 0.1arcsec texp ≈10 s
DKIST: a transformational facility
Weak quiet sun magnetic fields
DKIST as a coronagraph
High-grade polished M1 (~ 1 nm)
VBI
DKIST as a coronagraph
DL-NIRSPCryo-NIRSP
Coronal observat i ons and diagnost i c s in the IR (and visible) for DKIST first light
• Emphasis on bright line observations with greatest magnetic field sensitivityand IR.
• Corresponding peak temperature coverage: 1 to 1.6 MK.
Cryo-NIRSP Spectropolar.
Fe XIII λ10747Fe XIII λ10797He I λ10830Si X λ14300Si IX λ39350
Cryo-NIRSP Context Imager
Fe XIII λ10747He I λ10830Si IX λ39340
Maximum FOV: 5 arcmin Maximum FOV: 2.8 arcmin -- MulF -Instrument OperaF ons
DL-NIRSP Spectropolarimetry
Fe XI λ7892Fe XIII λ10747Fe XIII λ10797 He I λ10830Si X λ14300
VBI Imaging
Fe XI λ7892
VISP Spectropolarimetry
Various lines: 380 to 900 nm
DKIST Instrument Suite OverviewInstrument Name Acronym Wavelength Range AnalogsVisible Broadband Imager VBI
(blue, red)390 – 550 nm600 – 860 nm
Hinode/BFI; ROSAHigh cadence, high spa4al
res.
Visible Spectro-Polarimeter ViSP 380 – 900 nm SPINOR, Hinode/SP, IRIS
Scanning spectrograph, high spectral fidelity
Diffraction-Limited Near IR Spectro-Polarimeter
DL-NIRSP 500 – 900 nm900 – 1350 nm1350 – 1800 nm
SPIES, GRIS-IFUTrue IFU, variable spa4al
resolu4on / FOV
Visible Tunable Filter VTF 520 – 870 nm IBIS, CRISP, GFPI, HMIImaging spectro-polarimeter
Cryogenic Near IR Spectro-Polarimeter (with context imager)
Cryo-NIRSP 1000 – 5000 nm CYRA (BBSO)Cryogenic, scanning
spectrograph, novel IR diagnos4cs
What needs to be done (international collaboration)
• Leverage international collaboration (share expenses and responsibilities, prevent duplication, data sharing policies/international agreements, broaden international involvement)
• Ensure strong support from international societies (IAU, SCOSTEP/ICSU, WMO etc).
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Summary
• New groundbased instrument projects had been proposed in several countries (e.g., Brazil, China, EU, India, Hungary, Russia, USA)
• Several synoptic, long-term networks for research and space weather forecast are under development. Strong emphasis on space weather (but should we emphasize science aspects more?)
• Significant progress in derivation of coronal and chromosphericmagnetic field measurements (high resolution imaging and full Stokes Polarimetry in visible and near IR, full vector field in the chromosphere and corona; role of modeling in “inversion” of radio observations to derive magnetic field information).
• Close international collaboration is a key!
Thank you!
Sun CME Earth