new ground based instrument initiatives for solar and...
TRANSCRIPT
New ground based instrument initiatives for solar and solar terrestrial physics
Alexei A. Pevtsov (National Solar Observatory, USA)
goo.gl/LRVhVk
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)
goo.gl/LRVhVk
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).
goo.gl/LRVhVk
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