ASLAF: DETECTOR OF THE DIRECT SOLAR LYMAN- ALPHA RADIATION. FUTURE ALTERNATIVES V.Guineva(1), G.Witt(2), J.Gumbel(3), M.Khaplanov(3), R.Werner(1), J.Hedin(3),

Slides:



Advertisements
Similar presentations
New results of radiation environment investigation by Liulin-5 experiment in the human phantom aboard the International Space Station.
Advertisements

THE AURORAL EMISSIONS AND THE ELECTRON PRECIPITATION UNDER DIFFERENT GEOMAGNETIC CONDITIONS DURING RECURRENT SOLAR WIND STREAM Guineva V. 1, Despirak I.
Introduction to Plasma-Surface Interactions Lecture 6 Divertors.
Using a Radiative Transfer Model in Conjunction with UV-MFRSR Irradiance Data for Studying Aerosols in El Paso-Juarez Airshed by Richard Medina Calderón.
Chapter 23 Modern Earth Science
1 Ionospheres of the Terrestrial Planets Stan Solomon High Altitude Observatory National Center for Atmospheric Research
Modern Atmosphere and Air Pollution. Sunrise from space over the South China Sea. An astronaut would see something like this; clearly defined bands of.
METO621 Lesson 18. Thermal Emission in the Atmosphere – Treatment of clouds Scattering by cloud particles is usually ignored in the longwave spectrum.
PRECIPITATION OF HIGH-ENERGY PROTONS AND HYDROGEN ATOMS INTO THE UPPER ATMOSPHERES OF MARS AND VENUS Valery I. Shematovich Institute of Astronomy, Russian.
1.Solar-Terrestrial Influences Laboratory, BAS, Department Stara Zagora, Stara Zagora, Bulgaria 2. Solar-Terrestrial Influences Laboratory, BAS, Sofia,
1 Introduction to Plasma Immersion Ion Implantation Technologies Emmanuel Wirth.
METO 621 CHEM Lesson 7. Albedo 200 – 400 nm Solar Backscatter Ultraviolet (SBUV) The previous slide shows the albedo of the earth viewed from the nadir.
Atomic Absorption Spectroscopy (AAS)
The atmosphere surrounds Earth and protects us by blocking out dangerous rays from the sun. The atmosphere is a mixture of gases that becomes thinner.
Science Specification Table 12 keV keV for neutral particles 40.5 cm 2 image plane Electronic Noise 3 keV FWHM Proton Dead Layer
METO 621 Lesson 27. Albedo 200 – 400 nm Solar Backscatter Ultraviolet (SBUV) The previous slide shows the albedo of the earth viewed from the nadir.
MET 61 1 MET 61 Introduction to Meteorology MET 61 Introduction to Meteorology - Lecture 8 “Radiative Transfer” Dr. Eugene Cordero San Jose State University.
Lecture 1.3 – Structure of the Atmosphere. Today – we answer the following: How big is that atmosphere? Why is it like a cake? Why is cold in Denver?
The Atmosphere Layers Composition. Composition of “air” - What’s in it? Stable Components: N 2 78% O 2 21% CO 2 < 1% 100%
V. M. Sorokin, V.M. Chmyrev, A. K. Yaschenko and M. Hayakawa Strong DC electric field formation in the ionosphere over typhoon and earthquake regions V.
Ch. 5 - Basic Definitions Specific intensity/mean intensity Flux
621 project Spring project 1. The heating rate is defined as :- Let us assume that the effect of scattering is small, and that in the ultraviolet.
LIDAR: Introduction to selected topics
Dynamic thermal rating of power transmission lines related to renewable resources Jiri Hosek Institute of Atmospheric Physics, Prague, Czech Rep.
NATS 101 Lecture 2 Vertical Structure of the Atmosphere.
Stellar Atmospheres II
ON THE EFFICIENCY OF A LIDAR-TYPE SINGLE-SIDED GAMMA-RAY TOMOGRAPHY APPROACH Tanja Dreischuh, Ljuan Gurdev, Dimitar Stoyanov, Christo Protochristov*, Orlin.
M. Van Roozendael, AMFIC Final Meeting, 23 Oct 2009, Beijing, China1 MAXDOAS measurements in Beijing M. Van Roozendael 1, K. Clémer 1, C. Fayt 1, C. Hermans.
Elena Spinei and George Mount Washington State University 1 CINDI workshop March 2010.
Summarize the structure and composition of the atmosphere.
EARTH’S ATMOSPHERE. WHY IS IT IMPORTANT? Generate a classroom discussion.
Ion Beam Analysis of Gold Flecks in a Foam Lattice F E Gauntlett, A S Clough Physics Department, University of Surrey, Guildford, GU2 7XH, UK.
EARTH SCIENCE Prentice Hall EARTH SCIENCE Tarbuck Lutgens 
Introduction to Space Weather Jie Zhang CSI 662 / PHYS 660 Spring, 2012 Copyright © Ionosphere II: Radio Waves April 12, 2012.
Aerosol Limits for Target Tracking Ronald Petzoldt ARIES IFE Meeting, Madison, WI April 22-23, 2002.
Earth’s protective bubble
THE ATMOSPHERE (chapter 24.1)
Validation of OMI NO 2 data using ground-based spectrometric NO 2 measurements at Zvenigorod, Russia A.N. Gruzdev and A.S. Elokhov A.M. Obukhov Institute.
FIBER OPTIC TRANSMISSION
Chapter 23 The Atmosphere Section 1 Characteristics of Atmosphere Notes 23-2.
ESS 200C Lecture 13 The Earth’s Ionosphere
Transient response of the ionosphere to X-ray solar flares Jaroslav Chum (1), Jaroslav Urbář (1), Jann-Yenq Liu (2) (1) Institute of Atmospheric Physics,
1. The atmosphere 2 © Zanichelli editore 2015 Characteristics of the atmosphere 3 © Zanichelli editore 2015.
TEMPO Validation Capabilities Pandora NO 2 Total and tropospheric columns of NO2 from direct sun measurements -> column along a narrow cone (0.5 o ), actual.
Layers of the Atmosphere 1.  The atmosphere is divided into layers according to major changes in its temperature.  Gravity holds the layers of the atmosphere.
Atmosphere Layers. Vertical Structure of the Earth’s Atmosphere Vertical temperature (T) profile: troposphere stratosphere mesosphere Thermosphere (contains.
1 Atmospheric Radiation – Lecture 13 PHY Lecture 13 Remote sensing using emitted IR radiation.
Composition of the Atmosphere 14 Atmosphere Characteristics  Weather is constantly changing, and it refers to the state of the atmosphere at any given.
Layers of the Atmosphere
- 1 - Satellite Remote Sensing of Small Ice Crystal Concentrations in Cirrus Clouds David L. Mitchell Desert Research Institute, Reno, Nevada Robert P.
The Atmosphere The atmosphere is the layer of gases that surrounds the Earth. Earth’s atmosphere is a mixture of nitrogen, oxygen, water vapor, and many.
17 Chapter 17 The Atmosphere: Structure and Temperature.
Planck’s law  Very early in the twentieth century, Max Karl Ernest Ludwig Planck put forth the idea of the quantum theory of radiation.  It basically.
Remote sensing: the collection of information about an object without being in direct physical contact with the object. the collection of information about.
MICRO-STRIP METAL DETECTOR FOR BEAM DIAGNOSTICS PRINCIPLE OF OPERATION Passing through metal strips a beam of charged particles or synchrotron radiation.
Project presentation - Significant parameters for satellite communication.
17.1 Atmosphere Characteristics  D) Variable Components Water vapor 1) Water vapor is the source of all clouds and precipitation. water vapor absorbs.
Lecture 8: Stellar Atmosphere
The Atmosphere Layers Composition.
Aerosol extinction coefficient (Raman method)
Characteristics of the atmosphere
Planetary Ionospheres
Atmosphere: Origin, Composition and Structure
The Atmosphere of Earth
Atmosphere.
Layers of the atmosphere
By Narayan Adhikari Charles Woodman
Atmosphere: Origin, Composition and Structure
Layers of the atmosphere
Spectrophotometry A method to determine concentration of a species exploiting the absorption of EMR.
Presentation transcript:

ASLAF: DETECTOR OF THE DIRECT SOLAR LYMAN- ALPHA RADIATION. FUTURE ALTERNATIVES V.Guineva(1), G.Witt(2), J.Gumbel(3), M.Khaplanov(3), R.Werner(1), J.Hedin(3), S.Neichev(4), B.Kirov(5), L.Bankov(1), P.Gramatikov(4), V.Tashev(1), K.Hauglund(6), G.Hansen(6), J.Ilstad(6), H.Wold(6) 1)Solar-Terrestrial Influences Institute (STIL), Bulgarian Academy of Sciences (BAS)Stara Zagora Department, P.O.Box 73, 6000 Stara Zagora, Bulgaria; 2)Department of Earth Sciences, The Hebrew University (HUJI), Jerusalem, Israel; 3)Atmospheric Physics Group at the Department of Meteorology (MISU), Stockholm University, S Stockholm, Sweden; 4)Space Research Institute, Bulgarian Academy of Sciences (BAS), 6 Moskovska Str., 1000 Sofia, Bulgaria; 5)Solar-Terrestrial Influences Institute (STIL), Bulgarian Academy of Sciences (BAS), Acad. Georgi Bonchev Str., Block 3, 1113 Sofia, Bulgaria; 6)Andøya Rocket Range, Andenes, Norway Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

Basic scientific goal: Investigation of the processes in the mesosphere and the mesopause region by rocket measurements of the Lyman-alpha emission data. Research purposes of ASLAF Use of ASLAF instrument: for rocket measurements of the direct Lyman-alpha radiation penetrating in the atmosphere. Importance of a modern L  detector for rocket board measurements:  Acquiring the L  altitude profile and retrieval of the real O 2 concentration and temperature profiles;  Possibility to study the processes in the mesosphere and low thermosphere by analysis based on the obtained profiles. Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

TM Sun radiation Ion chamber Pre-amplifier + 2-stage amplifier Power supply U, T control Data channels ASLAF Principal scheme of the L  detector - ASLAF 2 data channels, x1 (15 nA) and x10 (1.5 nA); channels to monitor the power at the chamber (60V  1V) and the temperature. Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

ASLAF - Ionization chamber The ionization chamber is produced by the Artech corporation. Material: copper Weight: 50 g Max diameter: 30 mm Length: 36 mm Tubule: 32 mm MgF 2 window: diameter = 8 mm; sensitive to 105 – 135 nm radiation. Quantum efficiency: 40% - 60% for 25 V – 150 V Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

ASLAF - Ionization chamber Work values chosen: P = 20 mb (86% of L  are absorbed by estimation); U = 60 V; Imax = 15 nA (estimated current at the border of the atmosphere, direct Sun, Q=60%). Current through the ionization chamber, registered at different conditions – power supply and NO pressure. Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

Principal scheme of the electronic amplifier Sections: A1 - pre-amplifier and current-voltage converter; A2 – scaling and correcting amplifier; A3 – amplifies the signal 10 times; A4 – monitors the ionization chamber power supply; A5 – monitors the temperature. Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

ASLAF - Final design of the Lyman-alpha detector The maximal dimensions of the device are 105x60x90 mm, its weight is 498 g. Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

ASLAF response of the H lamp emission Linear signal depending on the emission intensity is obtained from both channels; The signal ratio can be considered 10.6 from 30 mV to 4.2 V in the channel 1.5 nA range. ASLAF – some characteristics Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

ASLAF – some characteristics ASLAF response to the produced electric current linearity constant signal ratio Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

ASLAF – some characteristics Signal test measurements from both channels Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

ASLAF – some characteristics Noise measurements, internal power on The noise in the Channel 15 nA is practically zero, and the one in Channel 1.5 nA is very low, with average value of 2.6 mV, what is near the sensitivity threshold. Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

ASLAF – some characteristics Angular dependence of the measured signal Fitting curve: Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

Data processing and analysis modeling the absorption process; obtaining the Lyman-alpha emission profile; computing the O 2 density, pressure and T profiles; comparing the obtained profiles with all other available measurements; analysis of the results. Consecutive steps: Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

Data processing and analysis Retrieval of the density, pressure and temperature profiles The photoabsorption cross-section σ is defined from where I 0 and I are the incident and transmitted intensities, n is the gas density, l is the path length and λ is the wavelength. For a mixture of gases we have – σ T, n T – total cross-section and number density; – n i, σ i, δ i – number density, cross-section and mixing ratio for the i th component. Assuming, that O 2 is the basic absorber, we can write: where f is a correction to include the absorption from other gases. Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

Data processing and analysis For a thin atmospheric layer with thickness dh and angle of the incident L  radiation θ the absorbed increment is: The total intensity is defined as Taking into account the pressure change across the layer, the expression for the pressure scale length H and its connection with the temperature the equations for n O2, p, and T can be derived. Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

Data processing and analysis Basic equations to compute the density, pressure and temperature profiles: Where the effective cross-section σ E, the level constant K and the ratio R are expressed by Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

Atmospheric model and quantities, to be used in the calculations: Plane-parallel atmosphere; Upper limit at 100 km; parallel homogeneous layers; Line-by-line calculations; Measured intensity in and outside of the atmosphere and shape of the Lyman-alpha line; The rocket coordinates and the corresponding position of the Sun towards it; The photoabsorption cross-section; The solar zenith angle θ. Data processing and analysis Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

Results and conclusions.  A modern Lyman-alpha detector (ASLAF) was designed and manufactured;  ASLAF passed successfully all tests performed before a rocket start;  The detector is an ionization chamber with work characteristics p=20 mb, U=60 V;  There are two measuring channels with ranges 1.5 nA and 15 nA, characterized with linearity, constant data ratio between them and low noise signal;  The channels monitoring the power supply to the ionization chamber and the temperature work well;  The power supply to the ionization chamber remain stable, 60V, with deviations from this value less then 1V;  The device is of very good quality and can be used in rocket experiments for measuring the L α flux. Lyman-alpha detector Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

1)Preparation for taking part in future rocket experiments with ASLAF (detector of the direct solar Lyman-alpha radiation); 2)Development of a new device to register the scattered solar Lyman-alpha radiation in the atmosphere; 3)Developing Lyman-alpha detector for satellite measurements; 4)Use of other, more sensitive detectors of Lyman-alpha radiation; 5)Improvement of the signal amplification and the power supply. Future alternatives: Results and conclusions. Workshop “Solar influences on the ionosphere and magnetosphere”, Sozopol, Bulgaria, 7-13 June 2009

Thanks for your attention !