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 * Home
    * Committee
    * Contact Us

 * Member Login
 * Courses
 * Radiofest
 * VK3RSP
 * Events
    * SPARC RadioFest 2022
    * SPARC John Moyle Field Day 2022
    * SPARC Christmas Party 2021
    * SPARC Bunnings Sausage Sizzle

 * Projects
 * Weather
    * Space Weather
    * SPARC Lightning tracker

 * Join SPARC


 * Home
   * Committee
   * Contact Us
 * Member Login
 * Courses
 * Radiofest
 * VK3RSP
 * Events
   * SPARC RadioFest 2022
   * SPARC John Moyle Field Day 2022
   * SPARC Christmas Party 2021
   * SPARC Bunnings Sausage Sizzle
 * Projects
 * Weather
   * Space Weather
   * SPARC Lightning tracker
 * Join SPARC

SPARC Solar Indices and Space Weather






Issued: 2023 Oct 18 0305 UTC by NOAA 
SFI: 137  The estimated planetary K-index at 0300 UTC on 18 October was 0.

Time UTC




CURRENT IMAGES OF OUR SUN

HMI Intensity

HMI Magnetogram

304 Angstroms

193 Angstroms – Coronal Holes

171 Angstroms




Space weather impacts radio communication in a number of ways. At frequencies in
the 1 to 30 MHz range (HF radio), the changes in ionospheric density and
structure modify the transmission path and even block transmission of HF radio
signals completely.



In the red image (304 Angstroms), we can see very small spicules—jets of solar
material—and some small prominences at the sun’s edge, which are not easy to see
in the other two images. In the second sequence (193 Angstroms), we can readily
observe the large and dark coronal hole, though it is difficult to make out in
the others. In the third image (171 Angstroms), we can see strands of plasma
waving above the surface.






SPACE WEATHER DESCRIBES THE VARIATIONS IN THE SPACE ENVIRONMENT BETWEEN THE SUN
AND EARTH.

In particular, Space Weather describes the phenomena that impact systems and
technologies in orbit and on Earth.






D REGION ABSORPTION PREDICTIONS (D-RAP)



There are several types of space weather that can impact HF radio communication.
In a typical sequence of space weather storms, the first impacts are felt during
the solar flare itself. The solar x-rays from the sun penetrate to the bottom of
the ionosphere (to around 80 km). There the x-ray photons ionize the atmosphere
and create an enhancement of the D layer of the ionosphere.



This enhanced D-layer acts both as a reflector of radio waves at some
frequencies and an absorber of waves at other frequencies. The Radio Blackout
associated with solar flares occurs on the dayside region of Earth and is most
intense when the sun is directly overhead.

CURRENT D REGION ABSORPTION PREDICTION






CURRENT SPACE WATHER OBSERVATIONS




SOLAR X-RAY FLUX



The GOES X-ray plots shown here are used to track solar activity and solar
flares. Large solar X-ray flares can change the Earth’s ionosphere, which blocks
high-frequency (HF) radio transmissions on the sunlit side of the Earth. Solar
flares are also associated with Coronal Mass Ejections (CMEs) which can
ultimately lead to geomagnetic storms.



While increasing SFI may be good for HF propagation, it also tends to correspond
with high Ap and K indices, which cause D-Layer absorption and noisy band
condition.



SOLAR PROTON FLUX



Protons are charged particles and are therefore influenced by magnetic fields



GEO MAGNETIC ACTIVITY



In a simplified view, geomagnetic activities are the product of the interaction
between the solar wind and magnetosphere. The Kp Index (p = planetary) is the
measure.



The K-index, and by extension the Planetary K-index, are used to characterize
the magnitude of geomagnetic storms. Kp is an excellent indicator of
disturbances in the Earth’s magnetic field and is used by SWPC to decide whether
geomagnetic alerts and warnings need to be issued for users who are affected by
these disturbances.



The principal users affected by geomagnetic storms are the electrical power
grid, spacecraft operations, users of radio signals that reflect off of or pass
through the ionosphere, and observers of the aurora.





24 HOUR SOLAR ACTIVITY SUMMARY



Issued: 2023 Oct 18 0030 UTC by NOAA 
 
Solar activity was low. Only three spotted regions remained on the solar
disk, all of which were stable and inactive. At about 17/0600 UTC, a CME
was observed following low level C-class activity near Region 3463 (S17,
L=180). Model results return a solution where the bulk of the ejecta
passes ahead of Earth, but some glancing influence may be possible on 21
Oct.

.Forecast...
Solar activity is expected to be low with a slight chance for R1-R2
(Minor-Moderate) events from 18-20 Oct.



Solar Summary Issued: 2023 Oct 18 0030 UTC by USAF/NOAA 
 
Regions with Sunspots.  Locations Valid at 17/2400Z 
Nmbr Location  Lo  Area  Z   LL   NN Mag Type
3464 N04W33   169  0090 Cso  06   07 Beta
3465 N10W10   146  0220 Cao  05   19 Beta
3468 S11E56   079  0130 Hax  01   01 Alpha
 
Regions Due to Return 18 Oct to 20 Oct
Nmbr Lat    Lo
3448 N13    012



LATEST VIDEO

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This channel highlights the outer atmosphere of the Sun – called the corona – as
well as hot flare plasma. Hot active regions, solar flares, and coronal mass
ejections will appear bright here. The dark areas – called coronal holes – are
places where very little radiation is emitted, yet are the main source of solar
wind particles.




THE SUN (EUV)





The GOES 16 and 17 spacecraft each carry a sophisticated extreme ultraviolet 
(EUV) telescope called the Solar Ultraviolet Imager (SUVI). This telescope
allows forecasters to monitor the Sun’s hot outer atmosphere or corona. EUV
photons are created in the million-degree plasma of the corona and are not
visible from the ground, due to the absorption of the Earth’s atmosphere.
Observations of solar EUV emission aids in the early detection of solar flares,
coronal mass ejections (CMEs), and other phenomena that impact the geospace
environment.

CORONAL MASS EJECTIONS





Coronal Mass Ejections (CMEs) are large expulsions of plasma and magnetic field
from the Sun’s corona. They can eject billions of tons of coronal material and
carry an embedded magnetic field (frozen in flux) that is stronger than the
background solar wind interplanetary magnetic field (IMF) strength. CMEs travel
outward from the Sun at speeds ranging from slower than 250 kilometres per
second (km/s) to as fast as near 3000 km/s. The fastest Earth-directed CMEs can
reach our planet in as little as 15-18 hours.

THE AURORA





This is a short-term forecast of the location and intensity of the aurora. This
product is based on the OVATION model and provides a 30 to 90 minute forecast of
the location and intensity of the aurora.

The aurora is an indicator of the current geomagnetic storm conditions and
provides situational awareness for a number of technologies.  The aurora
directly impacts HF radio communication and GPS/GNSS satellite navigation.  It
is closely related to the ground induce currents that impact electric power
transition.



Space weather can occur anywhere from the surface of the sun to the surface of
Earth. 



As a space weather storm leaves the sun, it passes through the corona and into
the solar wind. When it reaches Earth, it energizes Earth’s magnetosphere and
accelerates electrons and protons down to Earth’s magnetic field lines where
they collide with the atmosphere and ionosphere, particularly at high latitudes.



 Each component of space weather impacts a different technology.

Source: NOAA




SOLAR WIND

The Sun releases a constant stream of particles and magnetic fields called the
solar wind. This solar wind slams worlds across the solar system with particles
and radiation – which can stream all the way to planetary surfaces unless
thwarted by an atmosphere, magnetic field, or both. Here’s how these solar
particles interact with a few select planets and other celestial bodies. The
solar wind is mostly deflected by our magnetic field, but sometimes, when
intense, some of it can leak through. Once in near-Earth space, the particles
can trigger aurora near the poles.






GLOBAL IONOSPHERE

The top two panels show the latest global Total Electron Content (TEC) and
Maximum Usable Frequency (MUF) as forecasted by the WAM-IPE. The bottom two
panels show the anomaly in TEC and MUF taking the difference between the latest
values and a 10-day running average at the same universal time. The forecast is
updated with the latest real-time and forecast solar and geomagnetic drivers at
0, 6, 12 & 18 UT.



Click the image below to see a 3 day animation of the prediction.







HOW DOES SPACE WEATHER AFFECT US?



Space weather can present a serious hazard to today’s modern interconnected
society. This video from the Australian Bureau of Meterology explains how the
sun affects communications on Earth. Did you know that solar flares impact Earth
in less than 8 minutes? Particle radiation impacts between 10 minutes and
several hours, and a CME (Coronal Mass Ejection) typically arrives within 12 to
72 hours. What would happen here on Earth after a large event on the Earth
facing sun? This video explains the impact on our power grid, mobile phones,
internet, aviation, radio communications and more.




Source: SolarHam


MAXIMUM USEABLE FREQUENCY



The MUF map shows the Maximum Usable Frequency using colours and contour lines.
For example, if a given area on the map is greenish and lies between the
contours labelled “15” and “17”, then the MUF is around 16MHz in that location.
The readings from each individual station are shown as coloured dots with
numbers inside them, so you can see where the information is coming from. If a
dot is faded out, then that station currently has a low “confidence score”.
Source: prop.kc2g.com




A new map is generated every 15 minutes, from data that is usually between 5 and
20 minutes old. Therefore, on average, you’re looking at something based on
measurements taken about half an hour ago.



MUF is the highest frequency that is expected to bounce off of the ionosphere on
a path 3000km long. So the MUF along a path between two points shows the
possibility of long-hop DX between those points on a given band. If the MUF is
12MHz, then 30 meters and longer will work, but 20 meters and shorter won’t. For
long multi-hop paths, the worst MUF anywhere on the path is what matters. For
single-hop paths shorter than 3000km, the usable frequency will be less than the
MUF, because higher-angle signals “punch through” the ionosphere more easily. As
you get closer to vertical, the usable frequency drops to the Critical Frequency
(foF2). Source: prop.kc2g.com

Below is the current location of the moon and where it is visible on earth.
Handy for EME.







MEMBERSHIP INFO



Interested in becoming a member of SPARC? You're welcome to attend any club
function. Members meet each Thursday and Saturday from 9:30 am until 12:00 noon
with special lecture events and activities monthly. You can also participate in
our club nets held on Sunday mornings at 09:30 am on 146.675 MHz (88.5) and
Tuesday night on 3.640 MHz at 8pm.





SPARC REPEATER



VK3RSP, The SPARC 2 metre repeater is on 146.675 MHz. It's located on Arthurs
Seat which is the highest point on the Mornington Peninsula. A CTCSS tone of
88.5 Hz is required to access the device.




IRLP AND ECHOLINK



SPARC also provides a free access IRLP Node, 6330 connected via this repeater.
The repeater is also connected to Echolink node 290314 VK3RSP-R





CONTACT US



Postal Address:



P.O. Box 206 Rosebud

Victoria, 3939, AUSTRALIA



Email:



Please use the form on our contact us page.



Clubrooms:



Vern Wright Reserve Capel Sound





The Southern Peninsula Amateur Radio Club is incorporated in Victoria.
Registration Number: A0011981X

Club Constitution






Notifications