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

Presenter

Presentation Notes

Proposal was submitted for Horizon 2020; on US side we also submitted RFI to NSF

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