Medicane “Zorbas”

September 29th, 2018 |

NOAA-20 and Suomi NPP VIIRS Day/Night Band (0.7 µm) images [click to enlarge]

NOAA-20 and Suomi NPP VIIRS Day/Night Band (0.7 µm) images [click to enlarge]

Medicane “Zorbas” — as named by Freie Universität Berlin (surface analyses) — developed in the Mediterranean Sea late in the day on 27 September 2018. A toggle between VIIRS Day/Night Band (0.7 µm) images from NOAA-20 and Suomi NPP (above; courtesy of William Straka, CIMSS) revealed the well-defined circulation of the storm a few hours after Midnight local time on 28 September. Note the bright streak north of the storm center on the NOAA-20 image — this was an area of clouds illuminated by intense lightning activity. Other less prominent lightning streaks were evident in thunderstorms farther to the east over the Mediterranean Sea. On the Suomi NPP image, a small bright spot could be seen, evidence of minor volcanic activity at Mount Etna on the island of Sicily, as well as the hazy signature of a plume of blowing dust/sand that was moving northward off the coast of Libya. The corresponding VIIRS Infrared images are available here.

During the following daylight hours of 28 September, EUMETSAT Meteosat-11 High Resolution Visible (0.8 µm) images (below) showed the storm as it became better organized and increased intensity. Another dense plume of blowing dust/sand began to move off the coast of Libya late in the day.

Meteosat-11 Visible (0.8 µm) images, with hourly plots of wind barbs (yellow) and wind gusts (red) [click to play animation | MP4]

Meteosat-11 Visible (0.8 µm) images, with hourly plots of wind barbs (yellow) and wind gusts (red) [click to play animation | MP4]

On 29 September, Meteosat-11 Visible (0.8 µm) images (below) showed the Medicane moving inland along the Peloponnese coast of southern Greece — shortly after the storm center passed, winds gusted to 48 knots at Kalamata at 1220 UTC (while a heavy thunderstorm was being reported).

Meteosat-11 Visible (0.8 µm) images, with hourly plots of winds (yellow) and gusts in knots (red) [click to play animation | MP4]

Meteosat-11 Visible (0.8 µm) images, with hourly plots of wind barbs (yellow) and gusts in knots (red) [click to play animation | MP4]

A sequence of Terra and Aqua MODIS True Color Red-Green-Blue (RGB) images from 28 and 29 September from RealEarth (below) showed another view of the Zorbas on those 2 days (the valid time of the Terra MODIS image showing the eye-like feature on 29 September was 0911 UTC). Sea Surface Temperatures were near 25ºC in the central Mediterranean Sea where Zorbas was intensifying.

Terra/Aqua MODIS True Color RGB images on 28 and 29 September [click to enlarge]

Terra/Aqua MODIS True Color RGB images on 28 and 29 September [click to enlarge]

Hourly images of the MIMIC Total Precipitable Water product (below) showed moisture associated with the storm, which produced heavy rainfall and flash flooding in parts of southern Greece — the NESDIS Blended TPW Anomaly product indicated that this moisture was as much as 200% of normal for the region and date. Additional information and videos can be found here.

MIMIC morphed Total Precipitable Water images, 27-29 September [click to play animation | MP4]

MIMIC morphed Total Precipitable Water images, 27-29 September [click to play animation | MP4]

Hurricane Rosa

September 28th, 2018 |
GOES-15 Ifrared Window (10.7 µm, left) and GOES-17

GOES-15 Infrared Window (10.7 µm, left) and GOES-17 “Clean” Infrared Window (10.3 µm, right) images [click to play animation | MP4]

* GOES-17 images shown here are preliminary and non-operational *

GOES-15 (GOES-West) Infrared Window (10.7 µm) and GOES-17 “Clean” Infrared Window (10.3 µm) images (above) showed Hurricane Rosa on the morning of 28 September 2018, after it had rapidly intensified to Category 4 intensity overnight (ADT | SATCON). Since GOES-17 was operating in a Mode 6 scan strategy, images were available every 10 minutes (compared to every 15 minutes from GOES-15, with 30-minute gaps during Full Disk scans every 3 hours). A notable warming trend was seen in the cloud tops surrounding the eye.

A toggle between DMSP-18 SSMIS Microwave (85 GHz) and GOES-15 Infrared Window (10.7 µm) from the CIMSS Tropical Cyclones site (below) showed the bands of heavier precipitation withing the central dense overcast surrounding the eye at 1333 UTC.

DMSP-18 SSMIS Microwave (85 GHz) and GOES-15 Infrared Window (10.7 µm) images [click to enlarge]

DMSP-18 SSMIS Microwave (85 GHz) and GOES-15 Infrared Window (10.7 µm) images [click to enlarge]

After sunrise, a comparison of GOES-15 Visible (0.63 µm) and GOES-17 “Red” Visible (0.64 µm) images (below) revealed an eye that was filled with low-level clouds.

GOES-15 Visible (0.63 µm, left) and GOES-17 "Red" Visible (0.64 µm, right) images [click to play animation | MP4]

GOES-15 Visible (0.63 µm, left) and GOES-17 “Red” Visible (0.64 µm, right) images [click to play animation | MP4]

An animation of the MIMIC-TC product (below) showed that Rosa went through an eyewall replacement cycle during the morning, and was downgraded to a Category 3 intensity at 15 UTC.

MIMIC-TC morphed microwave product, 0000-1545 UTC [click to enlarge]

MIMIC-TC morphed microwave product, 0000-1545 UTC [click to enlarge]

Extratropical transition of Leslie

September 26th, 2018 |

GOES-16 Low-level (7.3 µm, left), Mid-level (6.9 µm, center) and Upper-level (6.2 µm, right) Water Vapor images [click to play animation | MP4]

GOES-16 Low-level (7.3 µm, left), Mid-level (6.9 µm, center) and Upper-level (6.2 µm, right) Water Vapor images [click to play animation | MP4]

GOES-16 (GOES-East) Low-level (7.3 µm), Mid-level (6.9 µm) and Upper-level (6.2 µm) Water Vapor images (above) showed Leslie as it transitioned from a Subtropical Storm at 00 UTC on 25 September to a Subtropical Depression at 03 UTC, then to a Post-Tropical Cyclone at 15 UTC, and eventually to a warm seclusion hurricane force cyclone with a classic “scorpion tail” sting jet signature by 00 UTC on 27 September.

Surface analyses during this 48-hour period are shown below; Leslie is located in the lower left corner. A longer animation (from 21-27 September) revealed the slowly-meandering circulation centers of pre- and post-Leslie (animated GIF | MP4).

Surface analyses at 6-hour intervals [click to play animation | MP4]

Surface analyses at 6-hour intervals [click to play animation | MP4]

The period of warm seclusion intensification of the remnants of Leslie, beginning after about 12-15 UTC on 26 September, was in response to the approach of an upper-level Potential Vorticity (PV) anomaly from the west-northwest (below). The “dynamic tropopause” — taken to be the pressure of the 1.5 Potential Vorticity Unit (PVU) surface — then descended to the 660 hPa pressure level (around 10,000 feet or 3 km) at 18 UTC on 26 September, according to GFS90 model fields.

GOES-16 Upper-level (6.2 µm) Water Vapor images, with contours of the PV1.5 pressure surface plotted in red [click to play animation | MP4]

GOES-16 Upper-level (6.2 µm) Water Vapor images, with contours of the PV1.5 pressure surface plotted in red [click to play animation | MP4]

GOES-16 Mid-level (6.9 µm) Water Vapor images, with contours of the PV1.5 pressure surface plotted in red [click to play animation | MP4]

GOES-16 Mid-level (6.9 µm) Water Vapor images, with contours of the PV1.5 pressure surface plotted in red [click to play animation | MP4]

GOES-16 Low-level (7.3 µm) Water Vapor images, with contours of the PV1.5 pressure surface plotted in red [click to play animation | MP4]

GOES-16 Low-level (7.3 µm) Water Vapor images, with contours of the PV1.5 pressure surface plotted in red [click to play animation | MP4]

This lowered tropopause brought ozone-rich air from the stratosphere down to very low altitudes — on GOES-16 Air Mass Red-Green-Blue (RGB) imagery (below), this ozone-rich air was highlighted by varying shades of red (the Air Mass RGB uses the 9.6 µm Ozone band to calculate the Green component).

GOES-16 Air Mass RGB images, with contours of PV1.5 pressure [click to play animation | MP4]

GOES-16 Air Mass RGB images, with contours of the PV1.5 pressure surface plotted in green [click to play animation | MP4]

A larger-scale view of the GOES-16 Air Mass RGB from the NWS Ocean Prediction Center (below) extends to 1115 UTC on 27 September.


An animation of the GOES-16 Air Mass RGB at 6-hour intervals from 00 UTC on 25 September to 12 UTC on 27 September is shown below, with and without contours of PV1.5 pressure. The dynamic tropopause descended to 850 hPa at 06 UTC on 27 September (when the storm was producing hurricane force winds) and eventually to 925 hPa at 12 UTC on 27 September (when it was producing storm force winds). The Air Mass RGB images highlighted the signature of the PV anomaly (shades of red) as it approached from the northwest then wrapped around the western and southern portion of the storm circulation.

GOES-16 Air Mass RGB images, with and without contours of GFS PV1.5 pressure [click to play animation | MP4]

GOES-16 Air Mass RGB images, with and without contours of GFS PV1.5 pressure [click to play animation | MP4]

The corresponding 6-hourly GOES-16 Split Water Vapor Difference (6.2 µm – 7.3 µm) images (below) show that a signature of the dry air aloft — associated with the aforementioned PV anomaly — was evident as a tongue of negative values in the -10 to -15ºC range (green to gray enhancement) that initially approached the storm from the northwest.

GOES-16 Split Water Vapor Difference (6.2 µm - 7.3 µm) images, with and without contours of PV1.5 pressure [click to play animation | MP4]

GOES-16 Split Water Vapor Difference (6.2 µm – 7.3 µm) images, with and without contours of PV1.5 pressure [click to play animation | MP4]

In cases such as this, the Air Mass RGB and Split Water Vapor Difference can be used in tandem to identify and track PV anomalies (18 UTC / 25 September | 12 UTC / 26 September). Note that east of the storm there also another small PV anomaly moving northward, associated with an upper-level low pressure feature — but this second PV anomaly played no role in the development/intensification of the post-tropical remnants of Leslie.

===== 27 September Update =====

Sequence of GOES-16 Low-level (7.3 µm), Mid-level (6.9 µm) and Upper-level (6.2 µm) Water Vapor images from 09 UTC on 27 September to 00 UTC on 28 September [click to play animation | MP4]

Sequence of GOES-16 Low-level (7.3 µm), Mid-level (6.9 µm) and Upper-level (6.2 µm) Water Vapor images from 09 UTC on 27 September to 00 UTC on 28 September [click to play animation | MP4]

A sequence of GOES-16 Low-level, Mid-level and Upper-level Water Vapor images from 09 UTC on 27 September to 00 UTC on 28 September (above) showed the classic wrapped dry/moist bands often seen with occluded mid-latitude cyclones.

GOES-17 Status and Transition to Operational GOES-West

September 26th, 2018 |

Graphic showing Pixel sizes for Bands 1, 3 and 5 (0.47 µm, 0.86 µm, and 1.61 µm) when GOES-17 is on station at 137º W Longitude. The GOES-West CONUS domain (where 5-minute scanning is routine) is shown in dashed white; GOES-West default Mesoscale Sectors (where 1-minute scanning is routine) are shown in solid white.

This blog post contains information on GOES-17 and its transition to the operational GOES-West satellite at 137º W Longitude (a link is here). Much as the Advanced Baseline Imager (ABI) imagery from GOES-17 is preliminary and non-operational, the information in this blog post is also preliminary, and it will be updated as needed.

The 16 ABI Channels all passed beta status in August. (At that point, GOES-17 data started flowing over the GOES Re-Broadcast [GRB]). Beta Provisional means that there are issues remaining in the individual channels, but they have been identified and are being addressed. Provisional status is expected to occur on 28 November 2018 this year — when the satellite is on station at 137 W. When that provisional status occurs, GOES-17 data will start flowing into NOAA’s CLASS archive (link).

NOAA/NESDIS announced on 26 September that the GOES-17 Drift from the test position at 89.5º W will start on 24 October 2018 at 1740 UTC, reaching its location as GOES-West (137º W) on 13 November 2018. Because ABI data are not transmitted when GOES-17 is moving, this means GOES-17 data will not be available for those 3 weeks. (When GOES-16 transitioned from the test position at 89.5º to its present GOES-East location at 75.2º, the data were missing for 14 days, from 30 November 2017 to 14 December 2017. GOES-17 will move at 2.5º per day, faster than GOES-16 did during its transition.

At about the same time that GOES-17 moves, GOES-15 will be shifted eastward from 135º W to 128º W. This shift starts 23 October 2018 at 2015 UTC and is predicted to end on 1 November 2018 at 1900 UTC. In contrast to GOES-R, however, GOES-15 can continue to transmit data as it moves. When GOES-15 is at its new location, the GOES-15 GVAR stream will be bounced off of GOES-14 (located at 105º W).

All 16 ABI Channels from 00:07 to 23:57 UTC on 30 August 2018 (Click to view mp4 animation)

The GOES-17 Advanced Baseline Imagery (ABI) is affected by malfunctioning Loop Heat Pipes (LHPs) on the spacecraft. Loop Heat Pipes dissipate heat, and because heat around the ABI is not dissipated, the energy emitted by the warmed satellite contaminates the ABI sensors: the ABI will measure energy coming from the Earth but also from the satellite itself. The bottom line is that during the night hours, the sun warms the satellite faster than it can cool.

The animation above (courtesy Tim Schmit, NOAA/NESDIS and CIMSS) shows the effects of the malfunctioning LHP on the worst day. During the night time, longwave infrared imagery (that is, longer than 3.9 µm) deteriorates in quality for several hours around local midnight. (The animation also includes a solar exclusion zone before that deterioration)   Before sunrise, as the ABI is shaded more and more by the GOES-17 spacecraft, the imagery becomes useable again.

This effect varies with season. The plot below (from Dan Lindsey, NOAA/NESDIS at CIRA), shows the solar declination with respect to the satellite. As the value gets smaller, solar forcing on the ABI increases. The minimum value would occur at Equinoxes, but the time around the Equinoxes is also Eclipse Season for the satellite: it moves through the Earth’s shadow around local midnight, and that passage through the shadow mitigates heating effects. Thus, the maximum solar forcing on the ABI occurs about 3.5 weeks before the Equinox, and again about 3.5 weeks after.

Sun angle at local midnight for GOES-17. Heating of the ABI is stronger as the angle decreases. Blue shading indicates Eclipse Seasons when solar forcing at satellite midnight is mitigated by the spacecraft’s passage through the Earth’s shadow. (Click to enlarge)

The plot below (courtesy Mat Gunshor, CIMSS) shows how the Focal Plane Module (FPM) Temperature changes as a function of time. Without solar forcing (that is, during the day when the ABI is in GOES-17’s shadow), the FPM temperature is around 80 K. At night, when sunlight hits ABI, FPM temperatures increase, and the peak value, around 105 K, happened at the end of August. A similar value will occur in October when Eclipse season is over.

Focal Plane Module Temperature for Longwave IR (Band 14), August through mid-September 2018 (Click to enlarge)

The reported effect of this extra heat on ABI data availability has evolved since May (when reports of data availability for only 12 hours were common), as a team of Scientists and Engineers from NOAA, NASA and Harris Company have gained a better understanding of the problem and how the effects of the heat can be mitigated. The current best estimates are that ABI Channels 7 (3.9 µm) and below (visible and near-infrared) will operate within design specifications throughout the year. The majority of the time will be when all channels provide good data throughout the day, but there will also be times, when solar forcing warms the ABI, that causes ABI data to be contaminated and likely unusable for a period around local satellite midnight (that is, midnight at 137 W Longitude). The water vapor channels (8, 9 and 10 at 6.19 µm, 6.95 µm, 7.34 µm), Ozone Channel (12, at 9.6 µm) and CO2 Channel (16, at 13.3 µm) will have 4-6 hours of bad or missing data; the infrared cloud phase/SO2 channel (11, at 8.46 µm) and the Dirty Window Channel (15, at 12.3 µm) will have around 3 hours of missing data; Window channels 13 and 14 (10.3 µm and 11.2 µm, respectively) will likely transmit useable data even during the warm season. However, data from those two window channels may be biased. This is all still under investigation, and these estimates are valid as of mid-September 2018. Scientists and engineers are still working to mitigate the problem and to adjust the way ABI is calibrated given the non-optimal operating temperature. The times of the year when data is most likely to be affected by LHP problems will be as the satellite approaches and exits Eclipse Seasons.

Top: GOES-17 Full Disk 12.3 µm Infrared Brightness Temperatures; Bottom: Time series of GOES-16 and GOES-17 Band 15 (12.3 µm) Brightness Temperatures averaged over a region (of size 401×401) centered over Florida from 00:02 UTC to 23:57 UTC on 30 August 2018 (Click to play mp4 animation)

The animation compares GOES-16 and GOES-17 “Dirty Window” 12.3 µm infrared brightness temperatures averaged in a 401×401-sized box centered over Florida.  There is excellent agreement before and after the issues associated with extra heating because of faulty LHPs.

Note that GOES-15 data may be used to supplement GOES-17 data during the times of data outage, although no decision has been made to operate GOES-15 long term.

Animations that show the evolution of the 16 channels through satellite midnight are available in PowerPoints here and here.