Personal Space Weather Station
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1 Personal Space Weather Station Nathaniel A. Frissell, W2NAF New Jersey Institute of Technology, K2MFF Special Thanks To Philip J. Erickson, W1PJE MIT Haystack Observatory Evan J. Markowitz, KD2IZW New Jersey Institute of Technology, K2MFF
2 What is Space Weather? Space weather is broad field, covering solar, heliospheric, magnetospheric, ionospheric physics, meteorology, aerospace engineering, etc... Definition: Space weather refers to conditions on the Sun and in the space environment that can influence the performance and reliability of space-borne and ground- based technological systems, and can endanger human life or health. [National Space Weather Program]
3 Where is Space Weather? Sun (Heliosphere) Solar Wind Magnetosphere Ionosphere Image Credit: NASA
4 What does Space Weather affect? Lou Lanzerotti/NJIT
5 But Space Weather? Or Climate? We talk about Space Weather all of the time. But really, we have some understanding of space climate, not space weather. Climate example: 11 Year Solar Cycle Ionosphere Day/Night Cycle Seasonal variations in propagation Weather example Solar flares Geomagnetic storms
6 Space Weather Station Goals Operations Research As hams building a Personal SW Station, what do we want to do? Hams: Know the best frequencies for working DX Understand the RFI Environment Communicate better during emergencies Scientists: Better sample the environment Better understand near-earth Space
7 Outline I. The Space Environment II. Traveling Ionospheric Disturbances III. My Vision of a Personal Space Weather Station IV. HF Receiver Instrument V. Project Goals and Timeline
8 The Space Environment
9 Solar-Terrestrial Environment NASA
10 Solar-Terrestrial Environment Steele Hill/NASA/NOAA
11 Sunspot Cycle
12 Solar Wind Over a Solar Cycle [McCommas et al., 2008, doi: /2008gl034896]
13 Differential Rotation [NASA]
14 Ionosphere
15 Skip Propagation Courtesy of Dec QST
16 Solar Wind & IMF Travel time to Earth: 2 to 4 days Magnetic field vector varies in magnitude & direction (~5 nt) Velocity: 300 to 800 km/s Density: 3 to 50 cm -3 Temperature: ~10 5 K [de Castro, 2008, doi: /s ]
17 Sun Facts The 11-year cycle is really a 22-year cycle (taking polarity flip into account) Total solar luminosity (dominated by visible light) varies only by ~0.1% Emission in UV & X-rays varies by orders of magnitude over the cycle. Sunspots Regions of strong magnetic field Dark because they are cool
18 NOAA Space Weather Prediction Center Global Scale Predictions Radio Blackouts Solar Radiation Storms Geomagnetic Storms
19 Solar Flares Sudden increase in electromagnetic energy from localized regions on the sun. Energy travels at the speed of light (8 min to Earth) Soft X-Ray ( nm) Earthward-directed energy can cause HF radio blackouts. Often, but not always, accompanied by a CME. NASA SDO Observation of X9.3 Solar Flare on Sept 6, 2017
20 Solar Radiation Storm Large-scale magnetic eruption on the sun accelerates charged particles to very high velocities. Associated with CMEs or Solar Flares Accelerated protons are most important 1/3 speed of light (100,000 km/s) 15 min to hours to reach Earth Guided by field lines into polar regions. Lasts for hours to days [NASA / Annotated by H. Singer]
21 Getting Energy into the Magnetosphere Southward IMF Solar Wind Nightside Reconnection Dayside Reconnection [Frissell, 2016, Dissertation]
22 Substorms [Visualization by NASA]
23 Magnetospheric Current Systems [Stern, 1994, doi: /94ja01239]
24 Geomagnetic Storms Fast CMEs and CIR/HSSs can lead to geomagnetic storms. Requires efficient energy exchange between solar wind and magnetosphere (extended periods of southward Bz and high-speed solar wind). Defined by negative excursion in Dst/Sym-H indices. Sym-H Magnetometers
25 Coronal Mass Ejections (CME) Large eruption of plasma and magnetic field from the solar corona. More common during solar maximum. Most distinguishing feature: A strong magnetic field with large out-of-the-ecliptic components. Speeds from 250 to 3000 km/s ( days to Earth). Slow CMEs merge into solar wind. Fast CMEs plow into solar wind and form shock waves. Temp [K] Speed [km/s] Density [cm -3 ] Bz [nt] Bx By Bt [nt] e7 1e6 1e5 1e ACE 13 July 2012 UT Hours
26 WSA-Enlil Model
27 High Speed Streams (HSSs) High Speed Streams are fast moving solar wind released from coronal holes. HSSs overtaking slow plasma creates compressed Corotating Interaction Regions Coronal holes Appear dark in EUV and soft X-ray because of cooler and less dense than surrounding plasma Regions of open, unipolar magnetic fields (this allows HSS to escape) More common during solar minimum Can last through several solar rotations [NASA SDO]
28 Geomagnetic Storm MIT Haystack Observatory / Anthea Coster
29 Ionospheric Storm Response [Thomas et al., 2016]
30 Kp/ap Index of geomagnetic perturbation Kp is logarithmic, ap is linear 3 hour resolution p stands for planetary Perturbations are normalized for each station before being combined into a planetary value. Kp ap Kp/Ap Magnetometers
31 Kp and the Auroral Oval [Signeres et a;, 2011, doi: /swsc/ ]
32 Auroral Electroject (AE/AL/AU) Auroral Electrojet indices senses auroral zone currents with ground magnetometers Auroral Upper (AU): Eastward Electrojet Auroral Lower (AL): Westward Electrojet Tracks substorm development AE = AU AL: Integrated auroral activity [Kamei, Sugiura, and Araki]
33 Auroral Electroject (AE/AL/AU/AO) 0746 UT
34 Space Weather and Ham Radio McMurdo Station, Antarctica KC4USV UT KC4USV khz
35 MSTID Science
36 Medium Scale Traveling Ionospheric Disturbances MSTIDs are a type of HF QSB [Samson et al., 1990]
37 Medium Scale Traveling Ionospheric Disturbances Ray trace simulation illustrating how SuperDARN HF radars observe MSTIDs. (a) Fort Hays East (FHE) radar field of view superimposed on a 250 km altitude cut of a perturbed IRI. FHE Beam 7 is outlined in bold. (b) Vertical profile of 14.5 MHz ray trace along FHE Beam 7. Background colors represent perturbed IRI electron densities. The areas where rays reach the ground are potential sources of backscatter. (c) Simulated FHE Beam 7 radar data, color coded by radar backscatter power strength. Periodic, slanted traces with negative slopes are the signatures of MSTIDs moving toward the radar. [Frissell et al., 2016]
38 MSTIDs Caused by Aurora? Svalbard, 2010, N. Frissell
39 MSTIDs Caused by Aurora? Except for point sources, it is very difficult to track any single MSTID over its entire lifetime. Observational papers generally report Equatorward propagation from high latitudes Lots of activity in fall and winter High and midlatitude MSTIDs are similar 1970s Theory Linked MSTIDs to Auroral AGWs Lorenz Forcing by Auroral Current Surges Joule Heating by Auroral Particle Precipitation [e.g., Chimonas and Hines, 1970; Francis, 1974]
40 MSTIDs Caused by Aurora? Many observational papers try to link MSTIDs to geomagnetic activity. Theory Equatorward propagation Originates from Auroral Zone Correlation of MSTID observations with space weather indices is marginal. If not the aurora, what else could it be? [Samson et al., 1989, 1990; Bristow et al., 1994, 1996; Grocott et al., 2013; Frissell et al., 2014]
41 Super Dual Auroral Radar Network SuperDARN Radar, McMurdo Station Antarctica Photo N. Frissell, 2014
42 Super Dual Auroral Radar Network 8-20 MHz OTH Radar 16 Antenna Linear Phased Array 4 Antenna Interferometer Array W per TX Multi-pulse sequence Measures Doppler Velocity Spectral Width SNR SuperDARN Radar, McMurdo Station Antarctica Photo N. Frissell, 2014
43 Super Dual Auroral Radar Network [Greenwald et al., 1995] 8-20 MHz OTH Radar 16 Antenna Linear Phased Array 4 Antenna Interferometer Array W per TX Multi-pulse sequence Measures Doppler Velocity Spectral Width SNR SuperDARN Radar, McMurdo Station Antarctica Photo N. Frissell, 2014
44 Super Dual Auroral Radar Network [ 15 Sept 2018]
45 Magnetospheric Convection The COMET Program / UCAR
46 Super Dual Auroral Radar Network SuperDARN Global Ionospheric Convection Maps
47 SuperDARN MSTID Study [Frissell et al., 2016]
48 Is it the Aurora? MSTID Active MSTID Quiet AE SYM-H
49 It s Cold Outside! NJIT Center for Solar-Terrestrial Research
50 MSTIDs Nov 2012 May 2013 Nov 2012 Dec 2012 Jan 2013 Feb 2013 Mar 2013 Apr 2013 May 2013 MSTID Active MSTID Quiet [Frissell et al., 2016]
51 Polar Vortex [Frissell et al., 2016]
52 Correlation with Polar Vortex! MSTID Active MSTID Quiet
53 Making a Discovery MSTID SuperDARN Science worked just by measuring amplitudes AND putting them into a coherent picture. SuperDARN SNR is NOT calibrated across radars Needed a way to normalize everything. We could still get good science out of that. By putting together a coherent picture from many sensors, we made a discovery! We could do the same with Ham Radio.
54 Development of Tornado Cell [Nishioka et al., 2013]
55 MSTID Resulting from Tornado [Nishioka et al., 2013]
56 MSTID Resulting from Tornado [Nishioka et al., 2013]
57 GPS-TEC vs SuperDARN TIDs
58 My Vision of a Personal Space Weather Station
59 Personal Terrestrial WX Station Multi-instrument Internet Connected Easy Set-Up Reasonable Cost Ambient Weather WS-2902
60 Personal Terrestrial WX Station Multi-instrument Internet Connected Easy Set-Up Reasonable Cost Can we build one for Space Weather? Ambient Weather WS-2902
61 Instrument Possibilities Ground Magnetometer? GPS-TEC Receiver? Ionosonde? Riometer? WWV/Standards Station Monitor? RBN/PSKReporter/WSPR Receiver? Lightning Detector? Others? What makes sense for a personal, ground-based local station?
62 Ground Magnetometers Detect Ionospheric & Space Currents Geomagnetic Storms Geomagnetic Substorms Kp and Ap are derived from GMAGs data.
63 GPS Total Electron Content Total Number of electrons between ground and GPS Satellite Measured by examining delay between two GPS Frequencies Traveling Ionospheric Disturbances Storm Effects Ionospheric Scintillations Courtesy of Anthea Coster
64 Ionosondes Vertical Incidence HF Radar Measure Plasma Density for bottomside Ionosphere Inverted Delta Transmit Anten San Juan Observatory (Small 15 m tall x 45 m long) Altitude [km] f pe 9 p n e [Dr. Terry Bullett, W0ASP, U of Colorado] Frequency [MHz]
65 Riometer Relative Ionopheric Opacity Meter Directly measures absorption of cosmic rays Indirectly measures electron density, particle precipitation Typically passive instrument MHz IRIS - Imaging Riometer for Ionospheric Studies in Finland ( Photo: Derek McKay
66 WWV/CHU Standards Monitor Steve Reyer, WA9VNJ
67 RBN/PSKReporter/WSPRNet RX [Frissell et al., 2014, Space Weather]
68 Lightning Detector Signatures from LF to VHF/UHF On HF, lightning noise can propagate long distances and disrupt communications Photo: Jessie Eastland (
69 Personal Space Weather Station Antenna GPS Disciplined Oscillator Software Defined Radio Radio Beacon Monitor RBN, PSKReporter, WSPR, Beacons HF Noise Characterizer GPS TEC Receiver Lightning Detector Traveling Ionospheric Disturbance Detector HamSCI Public Database Magnetometer Computer (e.g. Single Board Computer) Local User Display Local Data Reduction Sends Data to Server Internet
70 Some possible hardware Antenna DXE ARAV3? GPSDO Leo Bodnar? Magnetometer British Geological Survey? Software Defined Radio e.g. Red Pitaya? Computer e.g. Raspberry Pi? HamSCI Public Database Internet
71 Target Specifications Useful to ham radio, space science, and space weather communities. $100 to $500 (??) price range (accessible) Modular Instrument Design Easy ability to add or remove instruments, especially in software architecture Small footprint Nice User Interface/Local Display Standard format to send data back to a central repository Open community-driven design
72 Networking/Infrastructure App Ecosystem Publish/Subscribe? Data & Science Transfer Near real-time continuous monitoring Run Coordinated Campaign Request raw data from clients (Use ring buffer for past data) Retain ability to operate without Internet
73 Benefits to Owner PSWxS should also be useful to the local user/owner. Local display Web interface Ideas Identify which bands are active Characterize local RF environment Provide visual display of instrument data (both past and present) Act as a general receiver
74 HF Receiver Instrument
75 Where do we start? General purpose HF Receiving Instrument. Why? Few networks of widespread scientific HF radio receivers currently exist. Signals of opportunity available. Extremely flexible research tool. Directly applicable to ham radio. Radio is TAPR s Bread and Butter J
76 Where do we start? General purpose HF Receiving Instrument. Raw IQ MHz Well Calibrated and Documented
77 Where does this go? General purpose HF Receiving Instrument. Raw IQ MHz Well Calibrated and Documented Local Data Reduction Local Raw Recording (Ring Buffer) Always Sometimes HamSCI Public Database
78 Where does this go? General purpose HF Receiving Instrument. Raw IQ MHz Well Calibrated and Documented Local Data Reduction Local Raw Recording (Ring Buffer) Always Sometimes HamSCI Public Database
79 Quality Raw IQ is the Foundation Quality HF raw IQ à all downstream research and operational products.
80 HF Receiver Specifications What I Want Raw Spectrum from DC to Daylight Multiple Input Channels Absolute amplitude-calibrated receiver (i.e. Field Strength Meter) Calibrated system noise Accurate frequency resolution Accurate timing and location (enable interferometry) Known antenna system characteristics Infinite recording storage capacity
81 HF Receiver Specifications What I Want Reality/Implementation Raw Spectrum from DC to Daylight khz Slice Receivers Across HF Multiple Input Channels 2 Input Channels Absolute amplitude-calibrated receiver (i.e. Field Strength Meter) Calibrated system noise Inclusion of local, known noise source Accurate frequency resolution To accuracy provided by GPSDO Accurate timing and location (enable interferometry) To accuracy provided by GPSDO Known antenna system characteristics Provide recommendations to user Make easy for user to add metadata Infinite recording storage capacity Ring buffer Ability to request periods of raw data
82 Do things like this exist today? Not at a low to moderate cost Ettus has the performance, but not cost effective for this application Lots of choices of daughterboards/frequencies Ethernet interface Inputs for external 10 MHz and PPS Time stamps data
83 Measuring Noise Jim Frazier KC5RUO talked about issues of understanding noise in FT8/JT65/JT9 it s not easy! Exact numbers are less important (e.g. a wide variety of bandwidths can be used for the noise measurement as long as you know what you used!) Standardization and documentation is very important. Example noise sources Atmospheric Noise Lightning Noise Instrumental (self-generated noise) Cosmic noise
84 Measuring Noise Calibrated Local Noise Source P = K B T (BW) Could a reference noise source be integrated on the receiver board? ebay Millstone Hill ISR Radar Receiver RX Only RX + Noise Source
85 Importance of Metadata RF Instrument Metadata Center Frequency Bandwidth Impulse Response Sampling Fidelity (e.g. # of bits) Voltage to ADC Calibration Number Timestamp (UTC Locked) Station Metadata Station ID Station Configuration Geographic Location
86 MIT Haystack DigitalRF Software Provides a solution for storing all metadata with IQ data Uses standardized HDF5 data format GnuRadioSource and Sink Blocks Open Source
87 Project Goals and Timeline
88 Future Developments Software/Network Architecture Very Near Future Network Security Transmitter? Add instruments? Experimental features?
89 Eclipses 2023 and 2024 Eclipses in 2023 and 2024 are great targets for the Personal Space Weather Station Example Science Goal Look for TID wave signatures in both GPS-TEC and the HF receiver? [
90 Timeline Yr Date HF Rx Hardware Station Software Server Software 1 HamSCI 2019 Specifications & Initial Design TAPR 2019 Prototype Interface and Data Specification Interface and Database Specification 2 HamSCI 2020 Data Structure Implementation Database Implementation TAPR 2020 Beta Version Prototype Science/Eng Products Aggregate Data Test Science Products 3 HamSCI 2021 Refine Science/Eng Products Refine Science Products TAPR 2021 Field Tests Field Tests Field Tests 4 HamSCI 2022 Review & Refine Review & Refine Review & Refine TAPR 2022 Manufacture 5 HamSCI 2023 Distribute and Deploy TAPR 2023 Annular Eclipse 6 HamSCI 2024 Total Eclipse TAPR 2024 Analyze Data
91 Thank you!
92 Works Cited de Castro, Gómez, A.I. Astrophys Space Sci (2009) 320: Chimonas, G. & Hines, C. O. (1970), Atmospheric gravity waves launched by auroral currents, Planetary And Space Science, 18(4), , Francis, S. H. (1974), A Theory of Medium-Scale Traveling Ionospheric Disturbances, J. Geophys. Res., 79(34), , Frissell, N. A., Baker, J. B. H., Ruohoniemi, J. M., Gerrard, A. J., Miller, E. S., Marini, J. P., West, M. L., & Bristow, W. A. (2014), Climatology of medium-scale traveling ionospheric disturbances observed by the midlatitude Blackstone SuperDARN radar, Journal Of Geophysical Research: Space Physics, Frissell, N. A., Miller, E. S., Kaeppler, S. R., Ceglia, F., Pascoe, D., Sinanis, N., Smith, P., Williams, R., & Shovkoplyas, A. (2014), Ionospheric Sounding Using Real-Time Amateur Radio Reporting Networks, Space Weather, Frissell, N. A. (2016). Ionospheric Disturbances: Midlatitude Pi2 Magnetospheric ULF Pulsations and Medium Scale Traveling Ionospheric Disturbances (Doctoral dissertation, Virginia Tech), e.net/10919/ Frissell, N. A., J. B. H. Baker, J. M. Ruohoniemi, R. A. Greenwald, A. J. Gerrard, E. S. Miller, and M. L. West (2016), Sources and characteristics of medium-scale traveling ionospheric disturbances observed by high-frequency radars in the North American sector, J. Geophys. Res. Space Physics, 121, , doi: /2015ja Greenwald, R. A., Baker, K. A., Dudeney, J. R., Pinnock, M., Jones, T. B., Thomas, E. C., Villain, J.-P., Cerisier, J.-C., Senior, C., Hanuise, C., Hunsucker, R. D., Sofko, G., Koehler, J., Nielsen, E., Pellinen, R., Walker, A. D. M., Sato, N., & Yamagishi, H. (1995), DARN/SuperDARN: A global view of the dynamics of high-latitude convection, Space Sci. Rev., 71: , Grocott, A., Hosokawa, K., Ishida, T., Lester, M., Milan, S. E., Freeman, M. P., Sato, N., & Yukimatu, A. S. (2013), Characteristics of medium-scale traveling ionospheric disturbances observed near the Antarctic Peninsula by HF radar, Journal Of Geophysical Research: Space Physics, McComas, D. J., R. W. Ebert, H. A. Elliott, B. E. Goldstein, J. T. Gosling, N. A. Schwadron, and R. M. Skoug (2008), Weaker solar wind from the polar coronal holes and the whole Sun, Geophys. Res. Lett., 35, L18103, doi: /2008GL Nishioka, M., Tsugawa, T., Kubota, M., & Ishii, M. (2013), Concentric waves and short-period oscillations observed in the ionosphere after the 2013 Moore EF5 tornado, Geophysical Research Letters, 40(21), , Samson, J. C., Greenwald, R. A., Ruohoniemi, J. M., & Baker, K. B. (1989), High-frequency radar observations of atmospheric gravity waves in the high-latitude ionosphere, Geophys. Res. Lett., 16(8), , 008p Samson, J. C., Greenwald, R. A., Ruohoniemi, J. M., Frey, A., & Baker, K. B. (1990), Goose Bay Radar Observations of Earth-Reflected, Atmospheric Gravity Waves in the High- Latitude Ionosphere, J. Geophys. Res., 95(A6), , Sigernes, F., M. Dyrland, P. Brekke, S. Chernouss, D. A. Lorentzen, K. Oksavik, and C. S. Deehr (2011), Two methods to forecast auroral displays, J. Space Weather Space Clim., 1 (1) A03, DOI: /swsc/ Stern, D. P. (1994), The art of mapping the magnetosphere, J. Geophys. Res., 99(A9), , doi: /94JA Thomas, E. G., J. B. H. Baker, J. M. Ruohoniemi, A. J. Coster, and S.-R. Zhang (2016), The geomagnetic storm time response of GPS total electron content in the North American sector, J. Geophys. Res. Space Physics, 121, , doi: /2015J A
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