The COronal Diagnostic EXperiment (CODEX) is the solar coronagraph developed by NASA-Goddard Space Flight Center in collaboration with the Korea Astronomy and Space Science Institute (KASI), and the Italian National Institute for Astrophysics (INAF). CODEX will be launched in September 2024 and will be hosted by the International Space Station (ISS) as an external payload. CODEX is designed to observe the linearly polarized K-corona within the wavelength range 385-440 nm to obtain simultaneous measurements of density, temperature, and radial velocity of the coronal electrons. CODEX is a two-stage externally occulted coronagraph, with a field of view of 2.67 degrees, featuring two fold mirrors, and a series of occulting elements that minimize the amount of diffracted light reaching the detector. The polarization of the solar corona is measured by means of a commercial polarization image sensor manufactured by Sony, the IMX253MZR, that spatially modulates the incoming light beam. The polarimetric characterization of the instrument is one of the fundamental steps to derive the desired physical quantities of the solar corona from observations. It is hence crucial to understand how the instrument modifies the incident polarized light, especially due to the presence of the two fold mirror system within the light path, which is notoriously a source of polarization aberrations. This work describes the polarimetric characterization of the CODEX coronagraph, to determine an estimation of the instrumental polarization, and the results are presented.
The COronal Diagnostic EXperiment (CODEX) is a Heliophysics mission to measure the density, temperature, and velocity of the electrons in the solar corona with the primary goal of improving our understanding of the physical conditions of the solar wind in the acceleration region. The temperature and velocity measurement requires much higher signal-to-noise ratio than the density measurements. In solar coronagraphs, the diffraction of the solar disk light due to the occulting element is the dominant source of noise. Therefore, to further suppress the diffracted sun light with respect to the existing coronagraphs is a critical element of the CODEX design. To minimize the stray light due to diffraction, the selected optical design is a two-stage standard coronagraph with an external occulter, an internal occulter, and a Lyot stop. What is unique for this design is that a focal mask was inserted at the telescope focal plane. It works together with the field lens suppressing the stray light down by ~ another order of magnitude as compared to a traditional three-stage approach. During the optical design, a Fourier Transform based beam propagation software, i.e., GLAD, was used to model the beam path through the full coronagraph, from the external occulter to the detector array. All diffraction sensitive elements: external occulter, internal occulter, focal mask, and Lyot stop were carefully modeled and optimized. As a result, the requirement of achieving a stray light level which is one order of magnitude lower than F-corona was satisfied. On the other hand, to achieve the final suppression, a precision optical alignment is another must. This paper also presents our creative alignment procedure: using the combination of metrology, precision alignment equipment, and real time diffraction ring monitoring to minimize the diffraction. The final test results show that the suppression ratio (B/B0) reaches 10-11 level, which is equivalent to one order of magnitude lower than F-corona.
The Compact Doppler Magnetograph (CDM) is a space-qualified, miniaturized Doppler magnetograph, tailored to the requirements of a solar polar mission, and designed to provide photospheric line-of-sight magnetic field and Doppler velocity measurements of the solar surface. CDM is derived from the proven GONG (Global Oscillations Network Group) instrument design (Harvey et al., 1988, 1996), with a space qualified prototype developed for the Solaris solar polar MIDEX mission (Hassler et al., 2020). CDM has roughly 1/3 the mass of current state-of-the-art Doppler magnetographs (e.g., SOHO/MDI, SDO/HMI, SolO/PHI), with greatly increased sensitivity to the magnetic field (B) and Doppler velocity (v) and the capability to perform over an expanded spacecraft orbital velocity range, which is required to fit within the mission design constraints of currently feasible high latitude solar polar missions.
During the last two decades, Liquid Crystal Variable Retarder (LCVR) technology has matured and advanced as reliable and well-understood technology for ground applications to the point of being recently integrated in space-based optical instruments for the first time. LCVR cells use nematic liquid crystals to electronically tune the birefringence of the device in order to control the polarization of the transmitted light. The possibility to modulate the light polarization by means of an applied voltage offers the advantage of replacing the conventional rotary mechanisms, dedicated to carry the polarizing optics. Consequently, LCVR cells represent an excellent electro-optic solution to include in the design of space instruments where polarized light modulation is necessary. However, to validate the applicability of a LCVR cell to a space mission it is imperative to test its survivability in its exposure to conditions representative of the space environment. In this article, we summarize the activities performed to test the survivability of two commercial LCVR samples after their exposure to space-like environment for radiation and we report the result obtained by analyzing the radiation dose impact on the cell performances. The under-test samples have been produced by Meadowlark Optics Inc and designed for operation at 547 nm. We exposed the cells to multiple levels of gamma radiation dose, measuring their response time after each dose. To verify the impact of the accumulated radiation dose on the optical performances of the LCVR, we chose as indicators the retardance versus voltage, the transmission, and the response time. We measured these quantities before and after the whole test campaign and compared the two datasets to verify if gamma rays introduced any alterations in cell performances.
KEYWORDS: Coronagraphy, Diffraction, Vignetting, Signal to noise ratio, Point spread functions, Sensors, Polarization, Electrons, Solar processes, Temperature metrology
We are developing an innovative compact coronagraph for studying the physical conditions in the solar wind acceleration region. This paper presents the new development of the compact coronagraph for the investigation of temperature and speed of electrons in the solar corona. The proposed compact coronagraph is a one stage externally occulted coronagraph without internal occulter or Lyot stop mask. The key aspect of the new idea is to set the inner field cutoff at External Occulter (EO) much smaller than the specified inner field cutoff. A second occulter on the surface of the detector array removes the remaining diffraction. The occulter on the detector surface functions similar to an internal occulter with the Inner Field of View Cutoff (IFoVC) exactly the same as specified. For BITSE, the desired inner field cutoff is 3 R⊕, but the cutoff at EO is only 1.5 R. The diffraction analysis shows that in the sensor plane, the diffraction intensity at the 3 R is not sensitive to the EO cutoff, either at 1.5 R or close to 3 R. The advantage of having a smaller EO cutoff is that the vignetting decreased for the Field of View (FoV) near 3 R, therefore, the signal increases. Meanwhile, the diffraction of Point Spread Function is much less in the radial direction, which not only increases the image quality around 3 R, but also increases the encircled energy and signal to noise ratio. In other words, the data is useful right at 3 R! The BITSE optical design and diffraction analysis will be presented in detail. The simulation shows the signal to noise ratio obtained from the diffraction and vignetting data enables corona temperature and speed measurement.
The Heliospheric Imager (HI) is part of the SECCHI suite of instruments on-board the two STEREO observatories
launched in October 2006. The two HI instruments provide stereographic image pairs of solar coronal plasma and
coronal mass ejections (CME) over a field of view ranging from 13 to 330 R0.
The HI instrument is a combination of two refractive optical systems with a two stage multi-vane baffle system. The key
challenge of the instrument design is the rejection of the solar disk light by the front baffle, with total straylight
attenuation at the detector level of the order of 10-13 to 10-15. Optical systems and baffles were designed and tested to
reach the required rejection.
This paper presents the pre-flight optical tests performed under vacuum on the two HI flight models in flight temperature
conditions. These tests included an end-to-end straylight verification of the front baffle efficiency, a co-alignment and an
optical calibration of the optical systems. A comparison of the theoretical predictions of the instrument response and
performance with the calibration results is presented. The instrument in-flight photometric and stray light performance
are also presented and compared with the expected results.
HECOR (HElium CORonagraph) is a coronagraph designed to observe the solar corona at 30.4 nm between 1.2 and 4
solar radii. The instrument is part of the Herschel sounding rocket payload to be flown from White Sands Missile Range
in December 2007. Much like for neutral hydrogen, the residual singly ionized helium present in the corona can be
detected because it resonantly scatters the intense underlying chromospheric radiation. Combined with the simultaneous
measurements of the neutral hydrogen corona made by SCORE, the other coronagraph of the Herschel payload, the
HECOR observations will provide novel diagnostics of the solar wind outflow. HECOR is an externally occulted
coronagraph of very simple design. It uses a triple-disc external occulting system, a single off axis multilayer coated
mirror and a CCD camera. We present measurements of the EUV mirror roughness and reflectivity, tests of the image
quality, and measurements of the stray light rejection performance. The mirror uses a novel multilayer design with three
components that give HECOR a high throughput.
The Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) developed for the NASA Solar Terrestrial
Relations Observatory (STEREO) mission is a suite of optical telescopes that will, for the first time, observe the entire
inner heliosphere from the solar surface out to the vicinity of Earth from twin spacecraft. SECCHI was developed by an
international consortium led by the Naval Research Laboratory (NRL). The primary objective of the STEREO mission is
to understand the Coronal Mass Ejection (CME) phenomenon, discovered in 1971, and most recently extensively
observed by the NASA/ESA Solar and Heliospheric Observatory (SOHO). The SECCHI telescope suite is returning
unprecedented views of the Sun and inner heliosphere. The SECCHI instruments on each of the two STEREO spacecraft
observe CMEs from their initiation, through the corona, and into interplanetary space beyond the Earth's orbit. We
present an overview of the development and early operations of the SECCHI experiment.
The Heliospheric Imager (HI) forms part of the SECCHI suite of instruments aboard the two NASA STEREO spacecraft
which were launched successfully from Cape Canaveral AFB on 25 Oct 2006 (26 Oct UTC). Following lunar swingby's
on 15 Dec and 21 Jan respectively, the two spacecraft were placed in heliocentric orbits at approximately 1 AU - one
leading and one lagging the Earth, with each spacecraft separating from the Earth by 22.5° per year.
Each HI instrument comprises two wide-angle optical cameras - HI-1 and HI-2 have 20° and 70° fields-of-view which
are off-pointed from the Sun direction by 14.0° and 53.7° respectively, with the optical axes pointed towards the ecliptic
plane. In this way the cameras will for the first time provide stereographic images of the solar corona, and in particular of
Coronal Mass Ejections (CMEs) as they propagate outwards through interplanetary space towards the Earth and beyond.
The wide-field coverage of HI enables imaging of solar ejecta from 15 to about 330 solar radii whilst the other SECCHI
instruments (2 coronagraphs and an EUV imager) provide coverage from the lower corona out to 15 solar radii.
This paper briefly reviews the design and performance requirements for the instrument. The various activation, checkout
and calibration activities before and after opening the instrument's protective cover or door (instrument 'first-light') are
then described and it is shown that the instrument has met the design requirements, including CCD and camera imaging
performance, correction for shutterless operation of the cameras, straylight rejection and thermal requirements. It is
demonstrated from observations of a CME event on 24-25 Jan 2007 that the instrument is capable of detecting CMEs at
an intensity of 1% of the coronal background. Lessons learnt during the design, development and in-orbit operation of
the instrument are discussed.
The Solar Atmospheric Imaging Assembly (AIA) aboard the Solar Dynamics Observatory will characterize the dynamical evolution of the solar plasma from the chromosphere to the corona, and will follow the connection of plasma dynamics with magnetic activity throughout the solar atmosphere. The AIA consists of 7 high-resolution imaging telescopes in the following spectral bandpasses: 1215Å. Ly-a, 304 Å He II, 629 Å OV, 465 Å Ne VII, 195 Å Fe XII (includes Fe XXIV), 284 Å Fe XV, and 335 Å Fe XVI. The telescopes are grouped by instrumental approach: the MAGRITTE Filtergraphs (R. MAGRITTE, famous 20th Century Belgian Surrealistic Artist), five multilayer EUV channels with bandpasses ranging from 195 to 1216 Å, and the SPECTRE Spectroheliograph with one soft-EUV channel at OV 629 Å. They will be simultaneously operated with a 10-second imaging cadence. These two instruments, the electronic boxes and two redundant Guide Telescopes (GT) constitute the AIA suite. They will be mounted and coaligned on a dedicated common optical bench. The GTs will provide pointing jitter information to the whole SHARPP assembly. This paper presents the selected technologies, the different challenges, the trade-offs to be made in phase A, and the model philosophy. From a scientific viewpoint, the unique combination high temporal and spatial resolutions with the simultaneous multi-channel capability will allow MAGRITTE / SPECTRE to explore new domains in the dynamics of the solar atmosphere, in particular the fast small-scale phenomena. We show how the spectral channels of the different instruments were derived to fulfill the AIA scientific objectives, and we outline how this imager array will address key science issues, like the transition region and coronal waves or flare precursors, in coordination with other SDO experiments. We finally describe the real-time solar monitoring products that will be made available for space-weather forecasting applications.
The Extreme Ultraviolet Imager (EUVI) is part of the SECCHI instrument suite currently being developed for the NASA STEREO mission. Identical EUVI telescopes on the two STEREO spacecraft will study the structure and evolution of the solar corona in three dimensions, and specifically focus on the initiation and early evolution of coronal mass ejections (CMEs). The EUVI telescope is being developed at the Lockheed Martin Solar and Astrophysics Lab. The SECCHI investigation is led by the Naval Research Lab. The EUVI’s 2048 x 2048 pixel detectors have a field of view out to 1.7 solar radii, and observe in four spectral channels that span the 0.1 to 20 MK temperature range. In addition to its view from two vantage points, the EUVI will provide a substantial improvement in image resolution and image cadence over its predecessor SOHO-EIT, while complying with the more restricted mass, power, and volume allocations on the STEREO mission.
The ability to derive physical parameters of the Sun from observations by the Solar and Heliospheric Observatory (SOHO) Extreme Ultraviolet Imaging Telescope (EIT) greatly increases the scientific return of the mission. The absolute and time variable calibration of EIT therefore is of extreme interest. The NRL EIT Calibration Sounding Rocket (CalRoc) program was initiated to provide well calibrated, contemporaneous observations in support of SOHO EIT. These observations provide three benefits to the SOHO EIT data, absolute calibration points, temporal and spatial information of the EIT EUV response variability in flight via flat field information and clues to the physics of the degradation. Details of the bandpasses of the multilayered optics and the total telescope photometry are presented. Comparisons are shown with the contemporaneous images from SOHO EIT. Plans for the second CalRoc flight are discussed. Loss of reflectivity in the multilayer mirrors has been identified as a new component to the SOHO EIT and CalRoc degradation.
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