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© 2016 RAL Space
RAL Space and an Introduction to the
Worldwide IPS Stations (WIPSS) Network
M.M. Bisi ([email protected]) (1), J.A. Gonzalez-Esparza (2), B.V. Jackson (3),
E. Aguilar-Rodriguez (2), M. Tokumaru (4), I. Chashei (5), S.A. Tyul’bashev (5),
P.K. Manoharan (6), R.A. Fallows (7), M.A. Hapgood (1), R.A. Harrison (1),
O. Chang (8), J.C. Mejia-Ambriz (2), H.-S. Yu (3), K. Fujiki (4), and V. Shishov (5).
(1) STFC-RAL Space, Oxfordshire, UK. (2) SCIESMEX/MEXART/UNAM, Mexico.
(3) CASS-UCSD, CA, USA. (4) ISEE, Nagoya University, Japan.
(5) LPI-BSA, PRAO, Russia. (6) RAC-NCRA, TIFR, India.
(7) ASTRON, Dwingeloo, NL. (8) Posgrado en Ciencias de la Tierra, UNAM, Mexico.
© 2016 RAL Space
• Part 1: An Overview of Space Weather Interests/Activities
at RAL Space.
• Part 2: The Worldwide Interplanetary Scintillation
Stations (WIPSS) Network.
• Part 3: Brief Summary.
Outline…
STFC – Rutherford Appleton Laboratory
© 2016 RAL Space
World’s most powerful source of
pulsed neutrons
World’s first 3rd-generation
X-ray synchrotron
World’s most intense
laser
RAL Space
ECSAT + Sat Aps
Catapult
Our Ionospheric Physics Heritage: …the start of space environment physics at RAL
1924 - Radio Research Board formed, located at
Ditton Park Slough; Ionosphere discovered
and named by Appleton.
1927 - RADIO RESEARCH STATION established.
1931 - Ionosonde project starts (80+ years data and
running).
1935 - Invention of Radar at RRS by Watson Watt and
Wilkins.
1965 - RSS renamed the RADIO & SPACE
RESEARCH STATION.
1973 - RSRS renamed APPLETON LABORATORY
by Mrs M. Thatcher.
1980 - Appleton Lab. merges with Rutherford Lab..
1981 (to date) - EISCAT (and now EISCAT_3D).
1989-1991 - Cambridge IPS.
1990s onwards - Various satellite/space-based
involvements (e.g. ACE, CLUSTER, SWARM). © 2016 RAL Space
Our Solar/Heliospheric Physics Heritage: …the start of our space-based programme
© 2016 RAL Space
1958 - Plasma Spectroscopy Group set up at the Atomic
Energy Research Establishment, Harwell, for plasma
diagnostic analysis of ZETA (Zero Energy Toroidal
Assembly).
The UV spectroscopy techniques developed for ZETA
provided a powerful tool for studying astrophysical plasmas,
exploiting the new post-war rocket opportunities.
1962 - The group moved to Culham running a programme
of UV solar observations with rocket-borne
instruments, including the first flights of stabilised
Skylark rockets.
The Astrophysics Research Unit (as it was then) ultimately
became part of RAL.
1980s and 1990s - Key involvements in solar instrumentation
on SMM, Spacelab 2, and SOHO (still going today).
2000s and 2010s – Key involvements in solar/heliospheric
instrumentation on SMEI, STEREO, and Solar Orbiter.
► Research (10%)
Solar/Heliospheric Physics, I-R Astronomy, Space Weather, SST, Climate, Atmospheric Composition,
Radio Propagation…
► Design & build Space Instruments (50%)
216+ instruments in Space
plus Ground-based telescopes.
► Develop key technologies (15%)
Electronics/Detectors, Optics/Thermal, MMT, Robotics.
► Data and information Centres (25%)
Acquisition, Analysis, Dissemination, Curation.
© 2016 RAL Space
RAL Space – “Science Led, Technology Enabled”:
What we do…
Post Launch Support
(PLS)
LOFAR (from 2010): Low Frequency
Array radio telescope at the lowest
frequencies accessible from Earth. SOHO (from 1995): EUV
studies of the solar atmosphere.
STEREO (from 2006): Out of
Sun-Earth line heliospheric imaging.
Herschel (2009-2013): IR astronomical observatory.
Swarm (from 2013): Earth
magnetic field mission.
EISCAT (from 1981): Ionospheric radar.
Cluster (from 2000): The
near-Earth space environment.
Hinode (from 2006): Physics of the solar
atmosphere.
© 2016 RAL Space
Space-Weather Focus:
The Sun-Earth Connection
© 2016 RAL Space
Space weather arises (mainly) from solar
ejecta impacting the Earth, in particular
plasma and particle radiation.Need to understand energy flow:
Source (Sun) and transmission (solar wind), processing
by the Earth’s own magnetically-confined system
(magnetosphere, ionosphere/atmosphere, lithosphere).
Why is Space Weather a Natural
Hazard?
© 2016 RAL Space
Flooding People, homes, and infrastructure on flood plains and
coasts.
Tsunami People, homes, and infrastructure near coast.
Volcanoes People, homes, and infrastructure on pyroclastic and
lava flow lines.
Space weather People, homes and infrastructure near a star!
• Natural hazards occur in places that are good to live and occasionally
dangerous.
• Scale and frequency of extreme risks is a key concern.
Assessing the Risk• UK’s National Risk Register
(NRR – 2015 edition) –
other risks.
• Severe space weather has been
on the UK’s NRR since 2011.
• This, along with other additional
risks, were brought to the
government’s attention following
the problems caused by the
Iceland volcano ‘Eyjafjallajökull’
ash clouds in 2010.
• Not just the UK government!
• UKSA funded a socio-economic
study on space-weather impacts
(IPSP) reporting to government.
© 2016 RAL Space
Solar/Heliospheric Science
and Space Weather• Provide community focus.
• Design & build instruments/future technology.
• 10 Solar/Heliospheric missions over the last
30 years.
• Range of study:
– Physics & chemistry of the Sun to Solar activity,
Earth climate, and Space weather.
STEREO SDOHINODE Solar Orbiter
© 2016 RAL Space
Satellite
Ground station
Heliospheric Imaging• The disentangling of heliospheric structures
between the Sun and Earth is no simple task.
• There are many different features: different solar-wind streams,
stream interaction regions (SIRs), CMEs, etc…
• Remote-sensing heliospheric imaging via visible-light (Thomson
scattered sunlight off of heliospheric structures) or radio (indirect
via changes in signals from background sources) frequencies
enables us to get a good handle on the large space between Sun and
Earth (and beyond the Earth).
• Observations can be input into the University of California, San
Diego (UCSD) 3-D tomography for reconstruction (movie – top) of
the whole inner-heliospheric structure in several parameters…© 2016 RAL Space
Visible-Light Heliospheric Imaging
© 2016 RAL Space
• Earth-
directed
CME –
06 March
2012 as
imaged
by in
Thomson
-Scattered
sunlight.
Carrington-L5 Space-Weather Mission
• Prospects for a
UK/UK-led
dedicated space-
weather mission
to the Sun-Earth
Lagrangian 5
point (L5).
• Likely to be a
multi-national
endeavour if the
mission goes
ahead.© 2016 RAL Space
(Courtesy of
Airbus UK.)
Interplanetary Scintillation (IPS) (1)
© 2016 RAL Space
- e.g. see M.M. Bisi, “Planetary, heliospheric, and solar science with radio scintillation”,
Chapter 13 of Heliophysics Volume IV “Active stars, their astrospheres, and impacts on
planetary Environments”, Editors C.J. Schrijver, F. Bagenal, and J.J. Sojka,
Cambridge University Press, 16 March 2016, and references therein.
IPS (2)
IPS is most-sensitive at and around the P-Point of the LOS to the Sun and is only sensitive to the
component of flow that is perpendicular to the LOS; it is variation in intensity of astronomical
radio sources on timescales of ~0.1s to ~10s that is observed.
Interplanetary
magnetic field
Solar wind
velocity, density/
turbulence, and
signatures of field
rotation and SIRs
Variation in
amount of
scintillation →
density proxy
Cross-
correlation of
power spectra
→ velocityFit to individual power
spectra → velocity etc…
© 2016 RAL Space
WIPSS Core Members• M.M. Bisi – STFC RAL Space, UK.
• J.A. Gonzalez-Esparza, E. Aguilar-Rodriguez, O. Chang,
J.C. Mejia-Ambriz, V.H. De la Luz, P. Corona-Romero, and E.
Romero-Hernandez – SCIESMEX/MEXART/UNAM, Mexico.
• B.V. Jackson, and Hsiu-Shan Yu – CASS-UCSD, USA.
• M. Tokumaru, and K. Fujiki – ISEE, Nagoya University, Japan
• I.V. Chashei, S.A. Tyul’Bashev, V. Shishov – Pushchino Radio
Astronomy Observatory, Russia.
• R.A. Fallows – ASTRON, The Netherlands.
• P.K. Manoharan – Ooty Radio Telescope, India.
• Future expected additions (some are much more science
focused) from the Republic of Korea (South Korea)
(2016/2017), Ukraine (2017), China (2017), Australia (2017),
and perhaps South Africa (TBC).
Worldwide IPS Stations
(WIPSS) Network
Japan
Mexico
India
RussiaUK/Europe –
EISCAT/LOFAR
(USA-Australia)
Ooty 327 MHz、16,000 ㎡
Pushchino 111 MHz
70,000 ㎡MEXART
140 MHz、10,000 ㎡
MWA
80-300 MHz
ISEE Multi-Station 327 MHz
2000 ㎡× 3, 3500 ㎡
WIPSS
South
Korea
Low-Band Dipoles
~10 to 90 MHz.
High-Band Tiles
110 to ~250 MHz.
What we want from WIPSS (1)
© 2016 RAL Space
• Using the UCSD 3-D Tomography for real-time heliospheric
reconstruction and space-weather forecasting in this detail…
Overall Summary
• Part 1: RAL Space’s Space Weather Interests: Involves the whole
Sun-Earth chain; looking towards future ground-based and space-
based opportunities (including L5); and continuing working with
partners to emphasise and make the case for dedicated space-
weather missions and improvements to Sun-to-Earth modelling.
• Part 2: WIPSS Network: IPS is an extremely-powerful and unique
technique with a wide international interest for making heliospheric
imaging observations of the inner heliosphere as well as now
having validation for space-weather forecasting underway (RAL
Space/Met Office US Air Force EOARD project as well as several
international efforts); combined with heliospheric FR and the
UCSD tomography, this allows for huge potential in obtaining 3-D
magnetic-field forecasts as well as those in velocity and density.
© 2016 RAL Space