scholarly journals The Lyman-α Solar Telescope (LST) for the ASO-S mission

2015 ◽  
Vol 11 (S320) ◽  
pp. 436-438 ◽  
Author(s):  
Hui Li
Keyword(s):  
Spatial Resolution ◽  
White Light ◽  
Solar Flares ◽  
Solar Radius ◽  
Solar Observatory ◽  
Disk Center ◽  
Field Of View ◽  
Solar Telescope ◽  
The Sun ◽  
Full Disk

AbstractThe Lyman-α (Lyα) Solar Telescope (LST) is one of the payloads for the proposed Space-Borne Advanced Solar Observatory (ASO-S). LST consists of a Solar Disk Imager (SDI) with a field-of-view (FOV) of 1.2 R⊙ (R⊙ = solar radius), a Solar Corona Imager (SCI) with an FOV of 1.1 - 2.5 R⊙, and a full-disk White-light Solar Telescope (WST) with the same FOV as the SDI, which also serves as the guiding telescope. The SCI is designed to work in the Lyα (121.6 nm) waveband and white-light (for polarization brightness observation), while the SDI will work in the Lyα waveband only. The WST works in both visible (for guide) and ultraviolet (for science) broadband. The LST will observe the Sun from disk-center up to 2.5 R⊙ for both solar flares and coronal mass ejections with high tempo-spatial resolution

scholarly journals The Tor Vergata Synoptic Solar Telescope (TSST): A robotic, compact facility for solar full disk imaging

2020 ◽  
Vol 10 ◽  
pp. 58
Author(s):  
Luca Giovannelli ◽  
Francesco Berrilli ◽  
Daniele Calchetti ◽  
Dario Del Moro ◽  
Giorgio Viavattene ◽  
...  
Keyword(s):  
Solar Atmosphere ◽  
Space Weather ◽  
Coronal Mass Ejections ◽  
Low Cost ◽  
Optical Filter ◽  
Solar Telescope ◽  
The Sun ◽  
Weather Events ◽  
Line Observation ◽  
Full Disk

By the continuous multi-line observation of the solar atmosphere, it is possible to infer the magnetic and dynamical status of the Sun. This activity is essential to identify the possible precursors of space weather events, such as flare or coronal mass ejections. We describe the design and assembly of TSST (Tor Vergata Synoptic Solar Telescope), a robotic synoptic telescope currently composed of two main full-disk instruments, a Hα telescope and a Potassium (KI D1) magneto-optical filter (MOF)-based telescope operating at 769.9 nm. TSST is designed to be later upgraded with a second MOF channel. This paper describes the TSST concepts and presents the first light observation carried out in February 2020. We show that TSST is a low-cost robotic facility able to achieve the necessary data for the study of precursors of space weather events (using the magnetic and velocity maps by the MOF telescope) and fast flare detection (by the Hα telescope) to support Space Weather investigation and services.

scholarly journals On the peculiarities of manifestation of kG magnetic elements in observations of the Sun with low spatial resolution

2014 ◽  
Vol 10 (S305) ◽  
pp. 86-91 ◽  
Author(s):  
Mikhail L. Demidov ◽  
Renat M. Veretsky ◽  
Alexander V. Kiselev
Keyword(s):  
Magnetic Fields ◽  
Magnetic Flux ◽  
Spatial Resolution ◽  
Large Scale ◽  
Disk Center ◽  
Stellar Disk ◽  
The Sun ◽  
Surface Mapping ◽  
Cross Calibration ◽  
Stellar Magnetic Fields

AbstractOn the agenda of modern astrophysics is the exploration of not only disk-integrated stellar magnetic fields but surface mapping of them. However, it is hardly possible to expect that spatial resolution better than some dozens or hundreds pixels over stellar disk will be achieved for this goal in the foreseeable future. Among other reasons this fact makes very important observations of the average and large-scale magnetic fields of the Sun, which can be naturally used for testing polarimetric measurements on other stars, especially on solar-type stars. In this study we explore different aspects of observations of solar magnetic fields (SMF) with low spatial resolution, including Sun-as-a-star observations, which are characterized by extremely low magnetic flux densities. Comparison of disk-integrated and spatially resolved Stokes observations of the Sun allow us to demonstrate how Stokes V profiles depend on the distribution of large-scale magnetic fields in the disk center. It is shown that center-to-limb variations of magnetic strength ratios (MSR) and area asymetries, most likely could be interpreted as the manifestation of kG magnetic flux tubes. We have made cross-calibration of the full-disk magnetograms obtained by space-borned SDO/HMI and by the ground-based STOP telescope, and pretty good agreement is found. Finally, the absence of significant systematic time variations of MSRs with solar cycle is demonstrated.

New Initiatives for Synoptic Observations

2000 ◽  
Vol 179 ◽  
pp. 127-134
Author(s):  
C. U. Keller
Keyword(s):  
Solar Observatory ◽  
The Sun ◽  
National Solar Observatory ◽  
Synoptic Observations ◽  
Long Term Studies ◽  
Full Disk

AbstractSeveral new synoptic facilities for long-term studies of the Sun will become operational within the next few years. This paper summarizes information on some of these projects, in particular GONG+, ISOON, GOES/SXI, and SOUS. SOUS, the Synoptic Optical Long-Term Investigations of the Sun, is currently being built by the National Solar Observatory and will become operational in 2001. It consists of a 50-cm vector spectromagnetograph, a 14-cm full-disk patrol, and an 8-mm sun-as-a-star spectrometer.

scholarly journals HRTS Ultraviolet Solar Spectroscopy

1984 ◽  
Vol 86 ◽  
pp. 22-24 ◽  
Author(s):  
K.P. Dere
Keyword(s):  
High Resolution ◽  
Spatial Resolution ◽  
Wavelength Region ◽  
Solar Radius ◽  
The Sun ◽  
Video Cameras ◽  
Cassegrain Telescope ◽  
Film And Video

The NRL High Resolution Telescope and Spectrograph (HRTS) consists of a telescope, stigmatic UV spectrograph, UV broadband spectroheliograph and Hα film and video cameras. An image of the Sun is focussed onto the slit jaws of the spectrograph by a 30 cm Cassegrain telescope with a spatial resolution of 1". The stigmatic UV spectrograph employs a tandem-Wadsworth mount and photographically records spectra along the 1000" (1 solar radius) slit with a resolution of 50 mÅ in the 1170–1710 Å wavelength region. Images of the slit jaws in a tunable 100 Å bandpass are produced on film by the UV spectroheliograph which uses a reversed tandem-Wadsworth mount. The slit jaws are also viewed through an Hα filter by video and film cameras. To date, the HRTS instrument has flown on four rocket flights and is being prepared for flight on Spacelab-2.

scholarly journals The Design and Performance of the Gondola Pointing System for the Sunrise II Balloon-Borne Stratospheric Solar Observatory

2017 ◽  
Vol 06 (02) ◽  
pp. 1740007 ◽  
Author(s):  
A. Lecinski ◽  
G. Card ◽  
M. Knölker ◽  
B. Hardy
Keyword(s):  
Continuous Time ◽  
Digital Filters ◽  
Solar Observatory ◽  
Solar Telescope ◽  
The Sun ◽  
Sun Sensor ◽  
Convective Processes ◽  
Time Periods ◽  
And Performance ◽  
Better Than

With its 1[Formula: see text]m aperture, the Sunrise Balloon-Borne Stratospheric Solar Observatory was the largest space-based solar telescope. It was designed to study the magneto-convective processes of the sun at resolutions higher than 100[Formula: see text]km and the payload took data during a flight from June 12 to June 17, 2013. To achieve its science requirements, the telescope had to point to an accuracy of 26[Formula: see text] for extended periods of time. Pointing of the instrument was effected by the Sunrise Pointing System (PS). The PS used measurements provided by a Lockheed Intermediate Sun Sensor (LISS) and passed the data through a cascade of up to four digital filters to calculate the best voltages to drive the azimuthal and elevation motors. All filter settings could be modified in flight to adapt to changing conditions. Using this design, the PS met its requirements, pointing the instrument with an accuracy better than 26[Formula: see text] for 60% of the flight and for continuous time periods of up to 99[Formula: see text]min. In this paper, we detail the design and performance of the PS during the 2013 flight.

scholarly journals Present status of the Taiwan Oscillation Network

1997 ◽  
Vol 181 ◽  
pp. 31-38 ◽  
Author(s):  
Dean-Yi Chou ◽  
Keyword(s):  
Active Regions ◽  
Solar Observatory ◽  
The Sun ◽  
Subsurface Structure ◽  
Absorption Coefficients ◽  
High Resolution Data ◽  
Oscillation Network ◽  
Solar Intensity ◽  
Resolution Data ◽  
Full Disk

The Taiwan Oscillation Network (TON) is a ground-based network measuring solar intensity oscillations for the study of the internal structure of the Sun. So far, four telescopes have been installed at Teide Observatory (Tenerife), Huairou Solar Observing Station (near Beijing), Big Bear Solar Observatory (California), and Tashkent (Uzbekistan). The TON telescopes take K-line full-disk solar images of diameter 1000 pixels at a rate of one image per minute. The TON high-resolution data is specially suitable to study local helioseismology. Here, we present recent results of three topics on local helioseismology from TON data: (1) Inference of Subsurface Magnetic Field From Absorption Coefficients of p-modes in Active Regions, (2) Subsurface Structure of Emerging Flux Regions From Helioseismology, and (3) Flow Around Sunspots From Measurements of Frequency Shift.

scholarly journals Coordinated observations between China and Europe to follow active region 12709

2019 ◽  
Vol 15 (S354) ◽  
pp. 58-61
Author(s):  
S. J. González Manrique ◽  
C. Kuckein ◽  
P. Gömöry ◽  
S. Yuan ◽  
Z. Xu ◽  
...  
Keyword(s):  
Active Region ◽  
Imaging System ◽  
Broad Band ◽  
Solar Observatory ◽  
Disk Center ◽  
Solar Telescope ◽  
Band Filter ◽  
Small Pore ◽  
Polarity Inversion Line ◽  
Resolution Imaging

AbstractWe present the first images of a coordinated campaign to follow active region NOAA 12709 on 2018 May 13 as part of a joint effort between three observatories (China-Europe). The active region was close to disk center and enclosed a small pore, a tight polarity inversion line and a filament in the chromosphere. The active region was observed with the 1.5-meter GREGOR solar telescope on Tenerife (Spain) with spectropolarimetry using GRIS in the He i 10830 Å spectral range and with HiFI using two broad-band filter channels. In addition, the Lomnicky Stit Observatory (LSO, Slovakia) recorded the same active region with the new Solar Chromospheric Detector (SCD) in spectroscopic mode at Hα 6562 Å. The third ground-based telescope was located at the Fuxian Solar Observatory (China), where the active region was observed with the 1-meter New Vacuum Solar Telescope (NVST), using the Multi-Channel High Resolution Imaging System at Hα 6562 Å. Overlapping images of the active region from all three telescopes will be shown as well as preliminary Doppler line-of-sight (LOS) velocities. The potential of such observations are discussed.

scholarly journals Design of a Full Stokes Polarimeter for Chromospheric Measurements with SOLIS/VSM

2014 ◽  
Vol 10 (S305) ◽  
pp. 186-190
Author(s):  
S. Gosain ◽  
J. W. Harvey
Keyword(s):  
Magnetic Field ◽  
Solar Rotation ◽  
Solar Observatory ◽  
The Sun ◽  
Polarization Modulator ◽  
National Solar Observatory ◽  
Synoptic Observations ◽  
Stokes Polarimetry ◽  
Near Future ◽  
Full Disk

AbstractThe synoptic observations of the magnetic field of the Sun have continued at the National Solar Observatory (NSO) since 1970s. The daily full-disk maps of the longitudinal magnetic field are regularly combined to form Carrington maps of the photospheric magnetic flux per solar rotation. These maps continue to be used by the international research community for a variety of studies related to solar magnetism as well as for space weather studies. The current NSO synoptic facility is the Synoptic Optical Long-term Investigation of the Sun (SOLIS), which regularly provides photospheric vector and chromospheric longitudinal full-disk magnetograms, among other data products. In the near future, an upgrade of SOLIS to produce chromospheric vector magnetograms is planned. We present the design of a new polarization modulator package for full Stokes polarimetry of the chromospheric Ca II 854.2 nm spectral line.

scholarly journals On the manifestation in the Sun-as-a-star magnetic field measurements of the quiet and active regions

2010 ◽  
Vol 6 (S273) ◽  
pp. 56-60 ◽  
Author(s):  
Mikhail Demidov
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Large Scale ◽  
Active Regions ◽  
Field Measurements ◽  
Solar Observatory ◽  
Spectral Lines ◽  
The Sun ◽  
Time Data ◽  
Full Disk

AbstractThe best way to test the stellar magnetic field mapping codes is to apply them, with some changes, to the Sun, where high-precision disk-integrated and disk-resolved observations are available for a long time. Data sets of the full-disk magnetograms and the solar mean magnetic fields (SMMF) measurements are provided, for example, by the J.M.Wilcox Solar observatory (WSO) and by the Sayan Solar observatory (SSO). In the second case the measurements in the Stokes-meter mode simultaneously in many spectral lines are available. This study is devoted to analysis of the SSO quasi-simultaneous full-disk magnetograms and SMMF measurements. Changes of the SMMF signal with rotation of the surface large-scale magnetic fields are demonstrated. Besides, by deleting of selected pixels with active regions (AR) from the maps their contribution to the integrated SMMF signal is evaluated. It is shown that in some cases the role of AR can be rather significant.

The Optical Programme of the Culgoora Solar Observatory

1967 ◽  
Vol 1 (2) ◽  
pp. 39-40 ◽  
Author(s):  
R.G. Giovanelli
Keyword(s):  
Magnetic Field ◽  
High Resolution ◽  
Spatial Resolution ◽  
Solar Observatory ◽  
The Sun ◽  
Ionized Gas ◽  
Space And Time ◽  
Physical Quantities ◽  
Atmospheric Seeing

The Sun being a highly ionized gas, the basic physical quantities most needed for understanding solar phenomena are temperature, pressure (or density), velocity and magnetic field, together with their variations in space and time. The general aim at Culgoora is to secure observations from which these quantities may be derived (insofar as is practicable) simultaneously over extended solar regions. To do this has involved the development and use of filters of high spectral and spatial resolution, the study of atmospheric seeing and ways of securing high-resolution observations, and the study of methods of analysing observations to yield the physical quantities needed.

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