SH44B-1734
New Operational Modees of Linear-Electric-Field Time of Flight Telescopes
In situ measurements of space plasma have greatly improved our understanding of the space environment. For example, ion mass spectrometers that use electrostatic analyzers and time-of-flight systems enable researchers to identify revealing characteristics of ions in the solar wind. Using an optimized design of a linear-electric-field time-of-flight system, combined with a tophat electrostatic analyzer, we measure ions and make comparisons of resolution for both single and double-microchannel plate (MCP) configurations. The double-MCP design uses one MCP to detect straight-through particles and another to detect positive ions that experience isochronous time of flight. High mass resolution can be obtained because the isochronous ions are separated from their straight- through counterparts. In the single-MCP design, an isochronous ion will impact an emitting plate and send a secondary electron to the straight-through MCP. By focusing these secondary electrons and using position- sensitive detection, their signal can still be separated from particles that do not experience isochronous motion, thereby maintaining a high mass resolution. We also examine the ability to distinguish between molecules of similar mass, N2+ and CO+, by studying their atomic daughter products after breakup through a thin carbon foil.
SH44B-1735
An improved ACE/SWICS efficiency model including uncertainty estimates
SWICS (Solar Wind Ion Composition Spectrometer) is a linear time-of-flight mass spectrometer on ACE (Advanced Composition Explorer), launched 1997, and now at L1. SWICS determines the ion composition of the solar wind and of suprathermal particles in interplanetary space. For the purpose of an improved data analysis technique we have developed an advanced mathematical model of SWICS that calculates the detection probabilities as a function of ion species, energy, and flight trajectory. Based on careful analysis of calibration data and detailed comparison with flight data, we have included several effects in the model: Energy loss in the carbon foil was simulated with SRIM and adapted to flight and calibration results. Pulse height defects were derived from calibration data. Scattering in the foil has been improved by using results from dedicated scattering experiments performed at the University of Bern, Switzerland. Finally, we use the full 3-d information of the instrument to obtain accurate active areas. We present the operational breakdown of the efficiency model and the data products the program provides, and present uncertainty estimates for them.
SH44B-1736
Recent Developments in Transition Edge Strip Detectors for Solar X-Rays
LMSAL and NIST are developing position-sensitive X-ray strip detectors based on TES (Transition Edge Sensor) microcalorimeters optimized for solar physics. By combining high spectral (ΔE/E ~1600) and temporal (single photon Δt ~10μs) resolutions with imaging capabilities, these devices will be able to study high-temperature X-ray lines as never before. Diagnostics from these lines should provide significant new insight into the physics of both microflares and the early stages of flares. In this poster, we will discuss the status of our laboratory research, our most recent developments, and the applicability to future solar Explorers and other space missions.
SH44B-1737
The Astmospheric Imaging Assembly
The Atmospheric Imaging Assembly is a set of four EUV telescopes that will fly on the Solar Dynamic Observatory. The instrument has recently been delivered for integration to the Solar Dynamics Observatory. This poster provides an overview of the AIA instrument, its operation, and the data distribution plan. Pictures of the as delivery instrument are shown.
SH44B-1738
The High-resolution Lightweight Telescope for the EUV (HiLiTE)
The highly-structured and extremely dynamic interface between the photosphere and the corona is of crucial importance in understanding solar activity and space weather. Recent high-resolution observations with Hinode have shown that understanding this interface requires the ability to study the transition region by imaging plasma around 500,000 K on spatial scales of ~0.2 arc seconds, at cadences of ~5 seconds or less. We have completed a preliminary design of a telescope capable of meeting all three of these requirements - thermal, spatial, and temporal, called the High-resolution Lightweight Telescope for the EUV (HiLiTE). HiLiTE is a Cassegrain telescope with an aperture of 30 cm, angular resolution of ~0.2 arc seconds, and a mass that is about 1/4 that of one of the 20 cm aperture telescopes on SDO/AIA. The instrument bandpass will be tuned to the 46.5 nm Ne VII emission line formed in plasma at ~500,000 K. HiLiTE, including both mirrors and the metering structure, will be constructed entirely from lightweight, thermally stable, high-stiffness advanced Silicon Carbide (SiC) material. While SiC is an extremely promising material for space telescopes, SiC optics with the figure and surface finish required for normal-incidence multilayers have not yet been demonstrated. Upon integrating this instrument with an Advanced CMOS detector (in parallel development at Lockheed Martin via another internally funded program) and on board electronics, HiLiTE can easily be retrofitted to fly on board a sounding rocket, acting as a path finder to a post-AIA, Explorer-class mission. Herein, we give an update of the HiLiTE instrument development program, discussing expected instrument performance as well as the advantages of using SiC for EUV/Soft X-ray imaging in solar physics.