TY - JOUR
T1 - The Solar Activity Monitor Network
T2 - SAMNet
AU - Erdélyi, Robertus
AU - Korsós, Marianna B.
AU - Huang, Xin
AU - Yang, Yong
AU - Pizzey, Danielle
AU - Wrathmall, Steven A.
AU - Hughes, Ifan G.
AU - Dyer, Martin J.
AU - Dhillon, Vikram S.
AU - Belucz, Bernadett
AU - Brajša, Roman
AU - Chatterjee, Piyali
AU - Cheng, Xuewu
AU - Deng, Yuanyong
AU - Domínguez, Santiago Vargas
AU - Joya, Raúl
AU - Gömöry, Peter
AU - Gyenge, Norbert G.
AU - Hanslmeier, Arnold
AU - Kucera, Ales
AU - Kuridze, David
AU - Li, Faquan
AU - Liu, Zhong
AU - Xu, Long
AU - Mathioudakis, Mihalis
AU - Matthews, Sarah
AU - McAteer, James R.T.
AU - Pevtsov, Alexei A.
AU - Pötzi, Werner
AU - Romano, Paolo
AU - Shen, Jinhua
AU - Temesváry, János
AU - Tlatov, Andrey G.
AU - Triana, Charles
AU - Utz, Dominik
AU - Veronig, Astrid M.
AU - Wang, Yuming
AU - Yan, Yihua
AU - Zaqarashvili, Teimuraz
AU - Zuccarello, Francesca
N1 - Publisher Copyright:
© R. Erdélyi et al., Published by EDP Sciences 2022.
RE is grateful to the Science and Technology Facilities Council (STFC, grant numbers ST/M000826/1 and ST/V005979/1) the UK and the Royal Society for enabling this research. RE also acknowledges the CAS Presidents International Fellowship Initiative, Grant No. 2019VMA052 and the TOP CLLD 7.1.1-16-H-ERFA-2019-00207-Magyar Napfizikai Alaptvány ID Nr 1-8-2019/P support.MBK acknowledges STFC grant ST/S000518/1 to Aberystwyth University. MBK also acknowledges the open research program of CAS Key Laboratory of Solar Activity, National Astronomical Observatories, No. KLSA201610. RE and MBK both acknowledge the CAS Key Laboratory of Solar Activity, National Astronomical Observatories Commission for Collaborating Research Program for the support received to carry out part of this work. IGH and DP acknowledge support from EPSRC (grant EP/R002061/1). RB acknowledges the support by the Croatian Science Foundation under project 7549 “Millimeter and submillimeter observations of the solar chromosphere with ALMA”. RB, AH, and AMV acknowledge the support from the Austrian-Croatian Bilateral Scientific Project “Comparison of ALMA observations with MHD-simulations of coronal waves interacting with coronal holes”. AK and PG acknowledge the support from grant VEGA 2/0048/20. AAP acknowledges NASA 80NSSC18K1242 grant and grant No. 19-02-00088 by RFBR. Sunspot Solar Observatory is a partnership between NSF (1945705), the National Solar Observatory, the state of New Mexico, and consortium partners. TZ acknowledges funding from the Austrian Science Fund (FWF, project P30695-N27). FZ acknowledges support by the Università degli Studi di Catania (Piano per la Ricerca Università di Catania 2016–2018 – Linea di intervento 1 “Chance”; Linea di intervento 2 “Dotazione ordinaria”; Fondi di Ateneo 2020–2022, Università di Catania, Linea Open Access), by the Italian MIUR-PRIN grant 2017APKP7T on “Circumterrestrial Environment: Impact of Sun-Earth Interaction”. YH acknowledges funding from NSFC (11790300,11790301). DK has received funding from the Sêr Cymru II scheme, part-funded by the European Regional Development Fund through the Welsh Government. The editor thanks Stuart Jefferies and an anonymous reviewer for their assistance in evaluating this paper.
PY - 2022/1/26
Y1 - 2022/1/26
N2 - The Solar Activity Magnetic Monitor (SAMM) Network (SAMNet) is a future UK-led international network of ground-based solar telescope stations. SAMNet, at its full capacity, will continuously monitor the Sun’s intensity, magnetic, and Doppler velocity fields at multiple heights in the solar atmosphere (from photosphere to upper chromosphere). Each SAMM sentinel will be equipped with a cluster of identical telescopes each with a different magneto-optical filter (MOFs) to take observations in K I, Na D, and Ca I spectral bands. A subset of SAMM stations will have white-light coronagraphs and emission line coronal spectropolarimeters. The objectives of SAMNet are to provide observational data for space weather research and forecast. The goal is to achieve an operationally sufficient lead time of e.g., flare warning of 2–8 h and provide many sought-after continuous synoptic maps (e.g., LoS magnetic and velocity fields, intensity) of the lower solar atmosphere with a spatial resolution limited only by seeing or diffraction limit, and with a cadence of 10 min. The individual SAMM sentinels will be connected to their master HQ hub where data received from all the slave stations will be automatically processed and flare warning issued up to 26 h in advance.
AB - The Solar Activity Magnetic Monitor (SAMM) Network (SAMNet) is a future UK-led international network of ground-based solar telescope stations. SAMNet, at its full capacity, will continuously monitor the Sun’s intensity, magnetic, and Doppler velocity fields at multiple heights in the solar atmosphere (from photosphere to upper chromosphere). Each SAMM sentinel will be equipped with a cluster of identical telescopes each with a different magneto-optical filter (MOFs) to take observations in K I, Na D, and Ca I spectral bands. A subset of SAMM stations will have white-light coronagraphs and emission line coronal spectropolarimeters. The objectives of SAMNet are to provide observational data for space weather research and forecast. The goal is to achieve an operationally sufficient lead time of e.g., flare warning of 2–8 h and provide many sought-after continuous synoptic maps (e.g., LoS magnetic and velocity fields, intensity) of the lower solar atmosphere with a spatial resolution limited only by seeing or diffraction limit, and with a cadence of 10 min. The individual SAMM sentinels will be connected to their master HQ hub where data received from all the slave stations will be automatically processed and flare warning issued up to 26 h in advance.
KW - Sun-flares-precursors
UR - http://www.scopus.com/inward/record.url?scp=85121008118&partnerID=8YFLogxK
U2 - 10.1051/swsc/2021025
DO - 10.1051/swsc/2021025
M3 - Article
VL - 12
JO - Journal of Space Weather and Space Climate
JF - Journal of Space Weather and Space Climate
M1 - 2
ER -