Water: Sustained Flow

Nanedi Vallis: Sustained Water FLow?

Water Flow Evidence in Kasei Vallis

NASA’s Exploration Ground Systems conducts a water flow test with the mobile launcher at Kennedy Space Center’s Pad 39B in Florida on July 2, 2019. It is the first of nine tests to verify the sound suppression system is ready for launch of NASA’s Space Launch System for the first Artemis mission. During launch, 400,000 gallons of water will rush onto the pad to help protect the rocket, NASA’s Orion Spacecraft, mobile launcher, and launch pad from the extreme acoustic and temperature environment.

NASA’s Exploration Ground Systems conducts a water flow test with the mobile launcher at Kennedy Space Center’s Pad 39B in Florida on July 2, 2019. It is the first of nine tests to verify the sound suppression system is ready for launch of NASA’s Space Launch System for the first Artemis mission. During launch, 400,000 gallons of water will rush onto the pad to help protect the rocket, NASA’s Orion Spacecraft, mobile launcher, and launch pad from the extreme acoustic and temperature environment.

NASA’s Exploration Ground Systems conducts a water flow test with the mobile launcher at Kennedy Space Center’s Pad 39B in Florida on July 2, 2019. It is the first of nine tests to verify the sound suppression system is ready for launch of NASA’s Space Launch System for the first Artemis mission. During launch, 400,000 gallons of water will rush onto the pad to help protect the rocket, NASA’s Orion Spacecraft, mobile launcher, and launch pad from the extreme acoustic and temperature environment.

NASA’s Exploration Ground Systems conducts a water flow test with the mobile launcher at Kennedy Space Center’s Pad 39B in Florida on July 2, 2019. It is the first of nine tests to verify the sound suppression system is ready for launch of NASA’s Space Launch System for the first Artemis mission. During launch, 400,000 gallons of water will rush onto the pad to help protect the rocket, NASA’s Orion Spacecraft, mobile launcher, and launch pad from the extreme acoustic and temperature environment.

NASA’s Exploration Ground Systems conducts a water flow test with the mobile launcher at Kennedy Space Center’s Pad 39B in Florida on July 2, 2019. It is the first of nine tests to verify the sound suppression system is ready for launch of NASA’s Space Launch System for the first Artemis mission. During launch, 400,000 gallons of water will rush onto the pad to help protect the rocket, NASA’s Orion Spacecraft, mobile launcher, and launch pad from the extreme acoustic and temperature environment.

NASA’s Exploration Ground Systems conducts a water flow test with the mobile launcher at Kennedy Space Center’s Pad 39B in Florida on July 2, 2019. It is the first of nine tests to verify the sound suppression system is ready for launch of NASA’s Space Launch System for the first Artemis mission. During launch, 400,000 gallons of water will rush onto the pad to help protect the rocket, NASA’s Orion Spacecraft, mobile launcher, and launch pad from the extreme acoustic and temperature environment.

NASA’s Exploration Ground Systems conducts a water flow test with the mobile launcher at Kennedy Space Center’s Pad 39B in Florida on July 2, 2019. It is the first of nine tests to verify the sound suppression system is ready for launch of NASA’s Space Launch System for the first Artemis mission. During launch, 400,000 gallons of water will rush onto the pad to help protect the rocket, NASA’s Orion Spacecraft, mobile launcher, and launch pad from the extreme acoustic and temperature environment.

NASA’s Exploration Ground Systems conducts a water flow test with the mobile launcher at Kennedy Space Center’s Pad 39B in Florida on July 2, 2019. It is the first of nine tests to verify the sound suppression system is ready for launch of NASA’s Space Launch System for the first Artemis mission. During launch, 400,000 gallons of water will rush onto the pad to help protect the rocket, NASA’s Orion Spacecraft, mobile launcher, and launch pad from the extreme acoustic and temperature environment.

NASA’s Exploration Ground Systems conducts a water flow test with the mobile launcher at Kennedy Space Center’s Pad 39B in Florida on July 2, 2019. It is the first of nine tests to verify the sound suppression system is ready for launch of NASA’s Space Launch System for the first Artemis mission. During launch, 400,000 gallons of water will rush onto the pad to help protect the rocket, NASA’s Orion Spacecraft, mobile launcher, and launch pad from the extreme acoustic and temperature environment.

Nanedi Vallis: Sustained Water Flow? - High Resolution Image

About 450,000 gallons of water flowed at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers during a wet flow test at Launch Pad 39B at NASA's Kennedy Space Center in Florida. At peak flow, the water reached about 100 feet in the air above the pad surface. The test was a milestone to confirm and baseline the performance of the Ignition Overpressure/Sound Suppression system. During launch of NASA's Space Launch System rocket and Orion spacecraft, the high-speed water flow will help protect the vehicle from the extreme acoustic and temperature environment during ignition and liftoff.

About 450,000 gallons of water flowed at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers during a wet flow test at Launch Pad 39B at NASA's Kennedy Space Center in Florida. At peak flow, the water reached about 100 feet in the air above the pad surface. The test was a milestone to confirm and baseline the performance of the Ignition Overpressure/Sound Suppression system. During launch of NASA's Space Launch System rocket and Orion spacecraft, the high-speed water flow will help protect the vehicle from the extreme acoustic and temperature environment during ignition and liftoff.

About 450,000 gallons of water flowed at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers during a wet flow test at Launch Pad 39B at NASA's Kennedy Space Center in Florida. At peak flow, the water reached about 100 feet in the air above the pad surface. The test was a milestone to confirm and baseline the performance of the Ignition Overpressure/Sound Suppression system. During launch of NASA's Space Launch System rocket and Orion spacecraft, the high-speed water flow will help protect the vehicle from the extreme acoustic and temperature environment during ignition and liftoff.

About 450,000 gallons of water flowed at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers during a wet flow test at Launch Pad 39B at NASA's Kennedy Space Center in Florida. At peak flow, the water reached about 100 feet in the air above the pad surface. The test was a milestone to confirm and baseline the performance of the Ignition Overpressure/Sound Suppression system. During launch of NASA's Space Launch System rocket and Orion spacecraft, the high-speed water flow will help protect the vehicle from the extreme acoustic and temperature environment during ignition and liftoff.

About 450,000 gallons of water flowed at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers during a wet flow test at Launch Pad 39B at NASA's Kennedy Space Center in Florida. At peak flow, the water reached about 100 feet in the air above the pad surface. The test was a milestone to confirm and baseline the performance of the Ignition Overpressure/Sound Suppression system. During launch of NASA's Space Launch System rocket and Orion spacecraft, the high-speed water flow will help protect the vehicle from the extreme acoustic and temperature environment during ignition and liftoff.

TEST ENGINEER DENNIS STRICKLAND CONDUCTS WATER FLOW TESTS AT TEST STAND 116 FOR SPACE LAUNCH SYSTEM SCALE MODEL ACOUSTIC TEST SERIES (WITH SOLID ROCKET BOOSTERS)

TEST ENGINEER DENNIS STRICKLAND CONDUCTS WATER FLOW TESTS AT TEST STAND 116 FOR SPACE LAUNCH SYSTEM SCALE MODEL ACOUSTIC TEST SERIES (WITH SOLID ROCKET BOOSTERS)

TEST ENGINEER DENNIS STRICKLAND CONDUCTS WATER FLOW TESTS AT TEST STAND 116 FOR SPACE LAUNCH SYSTEM SCALE MODEL ACOUSTIC TEST SERIES (WITH SOLID ROCKET BOOSTERS)

jsc2022e072960 (9/16/2022) --- Front view of flow of mixture of hydrophobic medium sand particles, water, and air. After mixing hydrophobic medium sand particles with water and air, researchers flow the mixture through the pipe. Both agglomerates and excess free sand particles are visible. Researchers also observe the segregation phenomenon during the flow of this particular mixture. Agglomerates do not occupy the pipe uniformly and do not always flow at the same speed. Catastrophic Post-Wildfire Mudflows studies the formation and stability of this bubble-sand structure in microgravity. A better understanding of these phenomena could improve the understanding, modeling, and predicting of mudflows and support development of innovative solutions to prevent catastrophic post-fire events. Image courtesy of the UCSD Geo-Micromechanics Research Group.

A flow test of the Ignition Overpressure Protection and Sound Suppression water deluge system is underway on the mobile launcher at Launch Pad 39B at NASA's Kennedy Space Center in Florida, on July 25, 2019. The testing is part of a series of tests that Exploration Ground System is doing to verify the system is ready for the new Space Launch System rocket. Modifications were made to the pad after a previous wet flow test, increasing the performance of the system. During the launch of Artemis 1 and subsequent missions, this water deluge system will release about 450,000 gallons of water across the mobile launcher and Flame Deflector to reduce the extreme heat and energy generated by the rocket during ignition and liftoff.

A flow test of the Ignition Overpressure Protection and Sound Suppression water deluge system is underway on the mobile launcher at Launch Pad 39B at NASA's Kennedy Space Center in Florida, on July 25, 2019. The testing is part of a series of tests that Exploration Ground System is doing to verify the system is ready for the new Space Launch System rocket. Modifications were made to the pad after a previous wet flow test, increasing the performance of the system. During the launch of Artemis 1 and subsequent missions, this water deluge system will release about 450,000 gallons of water across the mobile launcher and Flame Deflector to reduce the extreme heat and energy generated by the rocket during ignition and liftoff.

A flow test of the Ignition Overpressure Protection and Sound Suppression water deluge system is underway on the mobile launcher at Launch Pad 39B at NASA's Kennedy Space Center in Florida, on July 25, 2019. The testing is part of a series of tests that Exploration Ground System is doing to verify the system is ready for the new Space Launch System rocket. Modifications were made to the pad after a previous wet flow test, increasing the performance of the system. During the launch of Artemis 1 and subsequent missions, this water deluge system will release about 450,000 gallons of water across the mobile launcher and Flame Deflector to reduce the extreme heat and energy generated by the rocket during ignition and liftoff.

A flow test of the Ignition Overpressure Protection and Sound Suppression water deluge system begins on the mobile launcher at Launch Pad 39B at NASA's Kennedy Space Center in Florida, on July 25, 2019. The testing is part of a series of tests that Exploration Ground System is doing to verify the system is ready for the new Space Launch System rocket. Modifications were made to the pad after a previous wet flow test, increasing the performance of the system. During the launch of Artemis 1 and subsequent missions, this water deluge system will release about 450,000 gallons of water across the mobile launcher and Flame Deflector to reduce the extreme heat and energy generated by the rocket during ignition and liftoff.

A flow test of the Ignition Overpressure Protection and Sound Suppression water deluge system is underway on the mobile launcher at Launch Pad 39B at NASA's Kennedy Space Center in Florida, on July 25, 2019. The testing is part of a series of tests that Exploration Ground System is doing to verify the system is ready for the new Space Launch System rocket. Modifications were made to the pad after a previous wet flow test, increasing the performance of the system. During the launch of Artemis 1 and subsequent missions, this water deluge system will release about 450,000 gallons of water across the mobile launcher and Flame Deflector to reduce the extreme heat and energy generated by the rocket during ignition and liftoff.

A flow test of the Ignition Overpressure Protection and Sound Suppression water deluge system is underway on the mobile launcher at Launch Pad 39B at NASA's Kennedy Space Center in Florida, on July 25, 2019. The testing is part of a series of tests that Exploration Ground System is doing to verify the system is ready for the new Space Launch System rocket. Modifications were made to the pad after a previous wet flow test, increasing the performance of the system. During the launch of Artemis 1 and subsequent missions, this water deluge system will release about 450,000 gallons of water across the mobile launcher and Flame Deflector to reduce the extreme heat and energy generated by the rocket during ignition and liftoff.

This image shows a plastic 1/48-scale model of an F-18 aircraft inside the "Water Tunnel" more formally known as the NASA Dryden Flow Visualization Facility. Water is pumped through the tunnel in the direction of normal airflow over the aircraft; then, colored dyes are pumped through tubes with needle valves. The dyes flow back along the airframe and over the airfoils highlighting their aerodynamic characteristics. The aircraft can also be moved through its pitch axis to observe airflow disruptions while simulating actual flight at high angles of attack. The Water Tunnel at NASA's Dryden Flight Research Center, Edwards, CA, became operational in 1983 when Dryden was a Flight Research Facility under the management of the Ames Research Center in Mountain View, CA. As a medium for visualizing fluid flow, water has played a significant role. Its use dates back to Leonardo da Vinci (1452-1519), the Renaissance Italian engineer, architect, painter, and sculptor. In more recent times, water tunnels have assisted the study of complex flows and flow-field interactions on aircraft shapes that generate strong vortex flows. Flow visualization in water tunnels assists in determining the strength of vortices, their location, and possible methods of controlling them. The design of the Dryden Water Tunnel imitated that of the Northrop Corporation's tunnel in Hawthorne, CA. Called the Flow Visualization Facility, the Dryden tunnel was built to assist researchers in understanding the aerodynamics of aircraft configured in such a way that they create strong vortex flows, particularly at high angles of attack. The tunnel provides results that compare well with data from aircraft in actual flight in another fluid-air. Other uses of the tunnel have included study of how such flight hardware as antennas, probes, pylons, parachutes, and experimental fixtures affect airflow. The facility has also been helpful in finding the best locations for emitting smoke from flight vehicles for flow vi

Kasei Valles is a valley system was likely carved by some combination of flowing water and lava. In some areas, erosion formed cliffs along the flow path resulting in water or lava falls. In some areas, erosion formed cliffs along the flow path resulting in water or lava falls. The flowing liquid is gone but the channels and "dry falls" remain. Since its formation, Kasei Valles has suffered impacts-resulting in craters-and has been mantled in dust, sand, and fine gravel as evidenced by the rippled textures. http://photojournal.jpl.nasa.gov/catalog/PIA20004

The teardrop-shaped island in this image was formed by the flow of fluid lava rather than liquid water

The dark, narrow streaks flowing downhill on Mars at sites such as this portion of Horowitz Crater are inferred to be formed by seasonal flow of water on modern-day Mars in this image from NASA Mars Reconnaissance Orbiter.

In this image from NASA Mars Odyssey spacecraft, numerous lava flows and fossae cracks are visible in a region of Mars located southeast of Olympus Mons. There is also a hint that water may have possibly flowed in the region.

Seasonal flows on warm Martian slopes may be caused by the flow of salty water on Mars, active today when the surface is warm above the freezing point of the solution. This observation is from NASA Mars Reconnaissance Orbiter.

The channels in this image from NASA Mars Odyssey spacecraftare located on the large volcanic flow complex north of Ascreaus Mons. The channels were carved by the flow of lava rather than water.

The channel in the bottom part of this image captured by NASA 2001 Mars Odyssey spacecraft was created by lava flow rather than water flow. This feature is located in the Tharsis plains east of Olympus Mons.

Among the many discoveries by NASA's Mars Reconnaissance Orbiter since the mission was launched on Aug. 12, 2005, are seasonal flows on some steep slopes. These flows have a set of characteristics consistent with shallow seeps of salty water. This July 21, 2015, image from the orbiter's High Resolution Imaging Science Experiment (HiRISE) camera shows examples of these flows on a slope within Coprates Chasma, which is part of the grandest canyon system on Mars, Valles Marineris. The image covers an area of ground one-third of a mile (536 meters) wide. These flows are called recurring slope lineae because they fade and disappear during cold seasons and reappear in warm seasons, repeating this pattern every Martian year. The flows seen in this image are on a north-facing slope, so they are active in northern-hemisphere spring. The flows emanate from the relatively bright bedrock and flow onto sandy fans, where they are remarkably straight, following linear channels. Valles Marineris contains more of these flows than everywhere else on Mars combined. At any season, some are active, though on different slope aspects at different seasons. Future human explorers (and settlers?) will need water to drink, grow food, produce oxygen to breath, and make rocket fuel. Bringing all of that water from Earth would be extremely expensive, so using water on Mars is essential. Although there is plenty of water ice at high latitudes, surviving the cold winters would be difficult. An equatorial source of water would be preferable, so Valles Marineris may be the best destination. However, the chemistry of this water must be understood before betting any lives on it. http://photojournal.jpl.nasa.gov/catalog/PIA19805

The force of moving water from a flood carved these teardrop-shaped islands within Granicus Valles. The orientation of the islands can be used as an indicator of the direction the water flowed. In this case, the water flowed primarily towards the upper left of the image. The image also contains many narrow sinuous channels. Geologists can determine that the floods occurred before a later tectonic event in the region. This event caused the crust to fracture into numerous blocks and fissures (grabens). Many fissures can be seen cutting across the former flood pathways. http://photojournal.jpl.nasa.gov/catalog/PIA04037

This artist concept illustrates how charged water particles flow into the Saturnian atmosphere from the planet rings, causing a reduction in atmospheric brightness.

This type of feature is termed an inverted channel. One theory of how these features form is that rocky debris accumulates in channels of flowing water beneath glaciers

Ares Vallis is a large valley that was carved billions of years ago by water flowing across the surface of Mars. This image shows an area where the flowing water may have stripped away some of the rocks and soils at the bottom of the valley, leaving behind the ridge-like formations. In other areas of our observation, such as the smooth terrain in the middle portion of this image, the flowing water appears to have carried in and left behind rocks and soils from somewhere upstream. Scientists study landforms, rocks and soils such as these to understand how, where and when floods occurred in Mars' past. https://photojournal.jpl.nasa.gov/catalog/PIA25551

This image from NASA 2001 Mars Odyssey spacecraft shows a small portion of Daedalia Planum, which is comprised of lava flows from Arsia Mons. Note the small channel in the image. This channel was likely created by lava rather than water flow.

The Tharsis region of Mars is covered in vast lava flows, many with channels. Some channels, however, resemble features that may have been formed by water. In this image, we see a smooth, flat-bottomed channel within the roughly irregular edges of a possible lava flow. This long, winding channel runs for 115 kilometers (70 miles) from its source (shown in ESP_045091_2045), maintaining a nearly consistent width. There is also a streamlined island within the channel, which is 1.25 kilometers (about 3/4 mile) long. One possibility is that a lava flow formed, and later groundwater was released, preferentially flowing through and further eroding the pre-existing lava channel. Or, the original lava flow could have been a very low-viscosity lava. We look at the shape and profile of the channel, and the channel and lava flow edges, to understand the characteristics of the fluids at work. Although there are lava flows and rivers on Earth that we can observe to understand the processes at work, the interplay of the features on Mars may tell a more complicated story. We want to be able to understand the history of volcanic activity in Tharsis, as well as possible interaction with ground water release, to better understand some of the younger landforms on Mars. http://photojournal.jpl.nasa.gov/catalog/PIA21104

This image shows the topography, with shading added, around the area where NASA Curiosity rover landed. An alluvial fan, or fan-shaped deposit where debris spreads out downslope, has been highlighted in lighter colors for better viewing.

This evenly layered rock photographed by the Mast Camera Mastcam on NASA Curiosity Mars Rover on Aug. 7, 2014, shows a pattern typical of a lake-floor sedimentary deposit not far from where flowing water entered a lake.

Streamlined islands, like the one shown in this NASA Mars Odyssey image, are one piece of geologic evidence that large quantities of water once flowed across the surface of Mars in the distant past.

The streamlined island in this image from NASA 2001 Mars Odyssey spacecraft formed within the channel of Maja Valles. The flow of water was deflected by the crater leaving material in the lee of the crater.

This image from NASA 2001 Mars Odyssey shows a complex region of channels in Tharsis. Called Olympica Fossae, these channel forms were created by lava flows rather than water.

Alluvial fans are gently-sloping wedges of sediments deposited by flowing water. Some of the best-preserved alluvial fans on Mars are in Saheki Crater, seen here by NASA Mars Reconnaissance Orbiter spacecraft.

This image from NASA 2001 Mars Odyssey spacecraft shows part of the eastern flank of Elysium Mons. The small channels were likely created due to the flow of lava, rather than water.

The channels in this image from NASA 2001 Mars Odyssey spacecraft were created by the flow of lava rather than water. These lava channels are near the northeast flank of Olympus Mons.

This image captured by NASA 2001 Mars Odyssey spacecraft shows several of the channels located in the Elysium Mons volcanic complex. It is likely that these channels were formed by lava flow rather than water.

This image from NASA Mars Reconnaissance Orbiter spacecraft the valley networks on Mars are terrains eroded by flowing water billions of years ago. Where bedrock is well exposed, a variety of colors due to altered minerals and polygonal patterns.

This observation from NASA Mars Reconnaissance Orbiter shows a small portion of Mawrth Vallis, one of the many outflow channels feeding north into the Chryse Basin. This ancient valley once hosted flowing water.

The channels in this image, taken by NASA 2001 Mars Odyssey spacecraft, are called Hephaestus Fossae and were most likely formed by lava flow and erosion rather than being eroded by water.

The channels in this image from NASA 2001 Mars Odyssey spacecraft are part of Granicus Valles. Granicus Valles is located just west of the Elysium Mons Volcanic Complex and was liked formed by the flow of lava rather than water.

This diagram depicts rivers entering a lake. Where the water flow decelerates, sediments drop out, and a delta forms, depositing a prism of sediment that tapers out toward the lake interior.

This image captured by NASA 2001 Mars Odyssey spacecraft shows a portion of Hebrus Valles. The flow of liquid water or lava is from the bottom of the image into the circular feature, which was likely filled by the material from the channel.

Given their location in the Tharsis volcanic complex, these channels were likely formed by the flow of lava rather than water in this image taken by NASA 2001 Mars Odyssey spacecraft.

Recurring slope lineae RSL may be due to active seeps of water. These dark flows are abundant along the steep slopes of ancient bedrock in Coprates Chasma as seen in this image from NASA Mars Reconnaissance Orbiter.

This anaglyph from NASA Mars Reconnaissance Orbiter spacecraft, shows that Eberswalde Delta contains river meanders, which indicate that flowing water was present for an extended period of time. 3D glasses are necessary to view this image.

NASA’s Exploration Ground Systems conducts a water flow test with the mobile launcher at Kennedy Space Center’s Launch Complex 39B in Florida on Oct. 24, 2023. It is the third in a series of tests to verify the overpressure protection and sound suppression system is ready for launch of the Artemis II mission. During liftoff, 400,000 gallons of water will rush onto the pad to help protect NASA’s SLS (Space Launch System) rocket, Orion spacecraft, mobile launcher, and launch pad from any over pressurization and extreme sound produced during ignition and liftoff.

NASA’s Exploration Ground Systems conducts a water flow test with the mobile launcher at Kennedy Space Center’s Launch Complex 39B in Florida on Oct. 24, 2023. It is the third in a series of tests to verify the overpressure protection and sound suppression system is ready for launch of the Artemis II mission. During liftoff, 400,000 gallons of water will rush onto the pad to help protect NASA’s SLS (Space Launch System) rocket, Orion spacecraft, mobile launcher, and launch pad from any over pressurization and extreme sound produced during ignition and liftoff.

NASA’s Exploration Ground Systems conducts a water flow test with the mobile launcher at Kennedy Space Center’s Launch Complex 39B in Florida on Oct. 24, 2023. It is the third in a series of tests to verify the overpressure protection and sound suppression system is ready for launch of the Artemis II mission. During liftoff, 400,000 gallons of water will rush onto the pad to help protect NASA’s SLS (Space Launch System) rocket, Orion spacecraft, mobile launcher, and launch pad from any over pressurization and extreme sound produced during ignition and liftoff.

NASA’s Exploration Ground Systems conducts a water flow test with the mobile launcher at Kennedy Space Center’s Launch Complex 39B in Florida on Oct. 24, 2023. It is the third in a series of tests to verify the overpressure protection and sound suppression system is ready for launch of the Artemis II mission. During liftoff, 400,000 gallons of water will rush onto the pad to help protect NASA’s SLS (Space Launch System) rocket, Orion spacecraft, mobile launcher, and launch pad from any over pressurization and extreme sound produced during ignition and liftoff.

NASA’s Exploration Ground Systems conducts a water flow test with the mobile launcher at Kennedy Space Center’s Launch Complex 39B in Florida on Oct. 24, 2023. It is the third in a series of tests to verify the overpressure protection and sound suppression system is ready for launch of the Artemis II mission. During liftoff, 400,000 gallons of water will rush onto the pad to help protect NASA’s SLS (Space Launch System) rocket, Orion spacecraft, mobile launcher, and launch pad from any over pressurization and extreme sound produced during ignition and liftoff.

NASA’s Exploration Ground Systems conducts a water flow test with the mobile launcher at Kennedy Space Center’s Launch Complex 39B in Florida on Oct. 24, 2023. It is the third in a series of tests to verify the overpressure protection and sound suppression system is ready for launch of the Artemis II mission. During liftoff, 400,000 gallons of water will rush onto the pad to help protect NASA’s SLS (Space Launch System) rocket, Orion spacecraft, mobile launcher, and launch pad from any over pressurization and extreme sound produced during ignition and liftoff.

The Tharsis region contains both large volcanoes and extensive lava plains. Most of the channel features in this region were formed by the flow of lava rather than the flow of water. Tectonic processes are also common and many linear depressions were created due to stresses in the Tharsis area as the surface expanded and lava forced its way to the surface to form volcanoes. This VIS image is located north of Jovis Tholus. Orbit Number: 73129 Latitude: 20.4782 Longitude: 241.464 Instrument: VIS Captured: 2018-06-09 15:55 https://photojournal.jpl.nasa.gov/catalog/PIA22667

This image from NASA Mars Reconnaissance Orbiter spacecraft shows a channel system flowing to the southwest toward the huge Hellas impact basin. We're not sure if this channel-inside-a-channel was carved by flowing water or lava. Flowing water erodes channels, and flowing lava both erodes and melts surrounding rock to form channels. It's not clear whether a huge surge of water or lava first formed the wide channel and then subsided into a trickle to form this narrow, inner channel, or if a trickle formed the inner channel and a subsequent surge formed the wider one. Detailed analysis of the shape could reveal which scenario is most likely, as well as whether water or lava is responsible. Relevant observations for such a determination would include, for example, the facts that the channels lack levees (ridges along the banks) and that the inner channel diverts around a mound, which at one time was an island. This channel system flowed to the southwest toward the huge Hellas impact basin.

A flow test of the Ignition Overpressure Protection and Sound Suppression water deluge system is in progress at Launch Pad 39B at NASA's Kennedy Space Center in Florida, on Oct. 15, 2018. At peak flow, the water reaches about 100 feet in the air above the pad surface. It flows at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers. The testing is part of Exploration Ground System's preparation for the new Space Launch System rocket. Modifications were made to the pad after a previous wet flow test, increasing the performance of the system. During the launch of Exploration Mission-1 and subsequent missions, this water deluge system will release about 450,000 gallons of water across the mobile launcher and Flame Deflector to reduce the extreme heat and energy generated by the rocket during ignition and liftoff.

A flow test of the Ignition Overpressure Protection and Sound Suppression water deluge system is in progress at Launch Pad 39B at NASA's Kennedy Space Center in Florida, on Oct. 15, 2018. At peak flow, the water reaches about 100 feet in the air above the pad surface. It flows at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers. The testing is part of Exploration Ground System's preparation for the new Space Launch System rocket. Modifications were made to the pad after a previous wet flow test, increasing the performance of the system. During the launch of Exploration Mission-1 and subsequent missions, this water deluge system will release about 450,000 gallons of water across the mobile launcher and Flame Deflector to reduce the extreme heat and energy generated by the rocket during ignition and liftoff.

A flow test of the Ignition Overpressure Protection and Sound Suppression water deluge system is in progress at Launch Pad 39B at NASA's Kennedy Space Center in Florida, on Oct. 15, 2018. At peak flow, the water reaches about 100 feet in the air above the pad surface. It flows at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers. The testing is part of Exploration Ground System's preparation for the new Space Launch System rocket. Modifications were made to the pad after a previous wet flow test, increasing the performance of the system. During the launch of Exploration Mission-1 and subsequent missions, this water deluge system will release about 450,000 gallons of water across the mobile launcher and Flame Deflector to reduce the extreme heat and energy generated by the rocket during ignition and liftoff.

A flow test of the Ignition Overpressure Protection and Sound Suppression water deluge system is in progress at Launch Pad 39B at NASA's Kennedy Space Center in Florida, on Oct. 15, 2018. At peak flow, the water reaches about 100 feet in the air above the pad surface. It flows at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers. The testing is part of Exploration Ground System's preparation for the new Space Launch System rocket. Modifications were made to the pad after a previous wet flow test, increasing the performance of the system. During the launch of Exploration Mission-1 and subsequent missions, this water deluge system will release about 450,000 gallons of water across the mobile launcher and Flame Deflector to reduce the extreme heat and energy generated by the rocket during ignition and liftoff.

A flow test of the Ignition Overpressure Protection and Sound Suppression water deluge system is in progress at Launch Pad 39B at NASA's Kennedy Space Center in Florida, on Oct. 15, 2018. At peak flow, the water will reach about 100 feet in the air above the pad surface. It will flow at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers. The testing is part of Exploration Ground System's preparation for the new Space Launch System rocket. Modifications were made to the pad after a previous wet flow test, increasing the performance of the system. During the launch of Exploration Mission-1 and subsequent missions, this water deluge system will release about 450,000 gallons of water across the mobile launcher and Flame Deflector to reduce the extreme heat and energy generated by the rocket during ignition and liftoff.

A flow test of the Ignition Overpressure Protection and Sound Suppression water deluge system is in progress at Launch Pad 39B at NASA's Kennedy Space Center in Florida, on Oct. 15, 2018. At peak flow, the water reaches about 100 feet in the air above the pad surface. It flows at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers. The testing is part of Exploration Ground System's preparation for the new Space Launch System rocket. Modifications were made to the pad after a previous wet flow test, increasing the performance of the system. During the launch of Exploration Mission-1 and subsequent missions, this water deluge system will release about 450,000 gallons of water across the mobile launcher and Flame Deflector to reduce the extreme heat and energy generated by the rocket during ignition and liftoff.

A flow test of the Ignition Overpressure Protection and Sound Suppression water deluge system is in progress at Launch Pad 39B at NASA's Kennedy Space Center in Florida, on Oct. 15, 2018. At peak flow, the water reaches about 100 feet in the air above the pad surface. It flows at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers. The testing is part of Exploration Ground System's preparation for the new Space Launch System rocket. Modifications were made to the pad after a previous wet flow test, increasing the performance of the system. During the launch of Exploration Mission-1 and subsequent missions, this water deluge system will release about 450,000 gallons of water across the mobile launcher and Flame Deflector to reduce the extreme heat and energy generated by the rocket during ignition and liftoff.

A flow test of the Ignition Overpressure Protection and Sound Suppression water deluge system begins at Launch Pad 39B at NASA's Kennedy Space Center in Florida, on Oct. 15, 2018. At peak flow, the water will reach about 100 feet in the air above the pad surface. It will flow at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers. The testing is part of Exploration Ground System's preparation for the new Space Launch System rocket. Modifications were made to the pad after a previous wet flow test, increasing the performance of the system. During the launch of Exploration Mission-1 and subsequent missions, this water deluge system will release about 450,000 gallons of water across the mobile launcher and Flame Deflector to reduce the extreme heat and energy generated by the rocket during ignition and liftoff.

41G-36-036 (5-13 Oct 1984) --- The deeply etched patterns of intermittent streams in the Hadhramaut Plateau of south Yemen. These stream beds, which now rarely carry water, are deeply entrenched, owing to the geologically recent uplift of the plateau. nonetheless, a very distinct watercourse appears along the top and bottom edges of the photograph. In the photograph's upper portion, available water will flow into the vast emptiness of the Rub al Khali (Empty Quarter). In the lower portion, water will flow to the Gulf of Aden.

This image from NASA's Mars Reconnaissance Orbiter (MRO) shows an impact crater looking amusingly like a tadpole because of the valley that was carved by water that used to fill it. It is often difficult to differentiate between inlet and outlet channels, but water always flows downhill. In this particular case, we can infer that water is flowing outward because we have the necessary terrain-height information. When studying these images in detail, scientists can gain a better understanding of the strength of the flooding water that carved the channels, and better understand the history of water activity in this region of Mars. https://photojournal.jpl.nasa.gov/catalog/PIA22241

Towards the top of this image from NASA 2001 Mars Odyssey spacecraft is a T shaped depression and two sections of narrow channel located on the northeast part of the Elysium Mons volcanic complex. Fluids like water, or lava flow downhill.

NASA Terra spacecraft shows the water flow after the U.S. Army Corps of Engineers opened the Morganza Spillway, a flood control structure along the western bank of the Mississippi River in Louisiana, to ease flooding along levee systems on May 14, 2011.

Florida Everglades is a region of broad, slow-moving sheets of water flowing southward over low-lying areas from Lake Okeechobeeto the Gulf of Mexico. These images fromNASA Terra satellite show the Everglades region on January 16, 2002.

Triangular shaped deposits at cliff edges are termed alluvial fans. Alluvial fans typically form in arid regions were water flow is limited, so deposits of material are not washed away as seen by NASA 2001 Mars Odyssey spacecraft.

This stereo image from the Mast Camera Mastcam on NASA Mars rover Curiosity shows a rock outcrop called Hottah, cited as evidence for vigorous flow of water in a long-ago Martian stream. You need 3D glasses to view this image.

Brown and tan muddy water flows down the Hudson River are seen in this image acquired by NASA Terra spacecraft on Sept. 1, 2011. After the torrential rains from Hurricane Irene, many rivers in the eastern United States were filled with sediment.

This image captured by NASA 2001 Mars Odyssey spacecraft shows where Patapsco Vallis enters the largest depression of Elysium Fossae. Patapsco Vallis, on the Elysium Mons volcanic complex, was likely formed by the flow of lava rather than water.

About 450,000 gallons of water flow at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers during a wet flow test on May 24, 2018, at Launch Pad 39B at NASA's Kennedy Space Center in Florida. At peak flow, the water reached about 100 feet in the air above the pad surface. The test was performed by Exploration Ground Systems to confirm the performance of the Ignition Overpressure/Sound Suppression system. During launch of NASA's Space Launch System rocket and Orion spacecraft, the high-speed water flow will help protect the vehicle from the extreme acoustic and temperature environment during ignition and liftoff.

About 450,000 gallons of water flow at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers during a wet flow test on May 24, 2018, at Launch Pad 39B at NASA's Kennedy Space Center in Florida. At peak flow, the water reached about 100 feet in the air above the pad surface. The test was performed by Exploration Ground Systems to confirm the performance of the Ignition Overpressure/Sound Suppression system. During launch of NASA's Space Launch System rocket and Orion spacecraft, the high-speed water flow will help protect the vehicle from the extreme acoustic and temperature environment during ignition and liftoff.

About 450,000 gallons of water flow at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers during a wet flow test on May 24, 2018, at Launch Pad 39B at NASA's Kennedy Space Center in Florida. At peak flow, the water reached about 100 feet in the air above the pad surface. The test was performed by Exploration Ground Systems to confirm the performance of the Ignition Overpressure/Sound Suppression system. During launch of NASA's Space Launch System rocket and Orion spacecraft, the high-speed water flow will help protect the vehicle from the extreme acoustic and temperature environment during ignition and liftoff.

About 450,000 gallons of water flow at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers during a wet flow test on May 24, 2018, at Launch Pad 39B at NASA's Kennedy Space Center in Florida. At peak flow, the water reached about 100 feet in the air above the pad surface. The test was performed by Exploration Ground Systems to confirm the performance of the Ignition Overpressure/Sound Suppression system. During launch of NASA's Space Launch System rocket and Orion spacecraft, the high-speed water flow will help protect the vehicle from the extreme acoustic and temperature environment during ignition and liftoff.

About 450,000 gallons of water flow at high speed from a holding tank through new and modified piping and valves, the flame trench, flame deflector nozzles and mobile launcher interface risers during a wet flow test on May 24, 2018, at Launch Pad 39B at NASA's Kennedy Space Center in Florida. At peak flow, the water reached about 100 feet in the air above the pad surface. The test was performed by Exploration Ground Systems to confirm the performance of the Ignition Overpressure/Sound Suppression system. During launch of NASA's Space Launch System rocket and Orion spacecraft, the high-speed water flow will help protect the vehicle from the extreme acoustic and temperature environment during ignition and liftoff.

The NASA SR-71A successfully completed its first cold flow flight as part of the NASA/Rocketdyne/Lockheed Martin Linear Aerospike SR-71 Experiment (LASRE) at NASA's Dryden Flight Research Center, Edwards, California on March 4, 1998. During a cold flow flight, gaseous helium and liquid nitrogen are cycled through the linear aerospike engine to check the engine's plumbing system for leaks and to check the engine operating characterisitics. Cold-flow tests must be accomplished successfully before firing the rocket engine experiment in flight. The SR-71 took off at 10:16 a.m. PST. The aircraft flew for one hour and fifty-seven minutes, reaching a maximum speed of Mach 1.58 before landing at Edwards at 12:13 p.m. PST. "I think all in all we had a good mission today," Dryden LASRE Project Manager Dave Lux said. Flight crew member Bob Meyer agreed, saying the crew "thought it was a really good flight." Dryden Research Pilot Ed Schneider piloted the SR-71 during the mission. Lockheed Martin LASRE Project Manager Carl Meade added, "We are extremely pleased with today's results. This will help pave the way for the first in-flight engine data-collection flight of the LASRE."

A flow test of the Ignition Overpressure Protection and Sound Suppression water deluge system begins at Launch Pad 39B at NASA's Kennedy Space Center in Florida, on Oct. 15, 2018. At peak flow, the water will reach about 100 feet in the air above the pad surface. The testing is part of Exploration Ground System's preparation for the new Space Launch System rocket. Modifications were made to the pad after a previous wet flow test, increasing the performance of the system. During the launch of Exploration Mission-1 and subsequent missions, this water deluge system will release about 450,000 gallons of water across the mobile launcher and Flame Deflector to reduce the extreme heat and energy generated by the rocket during ignition and liftoff.

Shown in this image from NASA's Mars Reconnaissance Orbiter (MRO) are alluvial fans, fan-shaped deposits emerging from regions of steep topography. Alluvial fans on Mars are thought to be ancient and record past episodes of flowing water. This image shows part of one of those fans, which has been eroded. The old stream channels now stand above the rest of the fan as ridges, mostly in the southern (bottom) part of the image. This can occur because the channel materials are more resistant to erosion; perhaps they had larger grains (gravel) or because minerals deposited from the water cemented together. https://photojournal.jpl.nasa.gov/catalog/PIA22332

Alluvial fans are piles of debris dumped by rivers when they emerge from the mountains and enter a mostly dry valley as seen by NASA Mars Reconnaissance Orbiter. A bajada (such as this example named after the famous American filmmaker) consists of a series of coalescing alluvial fans along a mountain front. On the surface of this bajada, one can see many sinuous ridges. These ridges mark the path that streams of water took as they flowed into this crater. The sinuosity of the ridges tells us something about the speed of the water flow. Fast moving flows tend to be straighter than slow-moving. Observations like this help us build a picture of how rivers behaved on ancient Mars. http://photojournal.jpl.nasa.gov/catalog/PIA19366

The central portion of this image features a mildly-winding depression that was carved by water, likely around four billion years ago shortly after the Hellas basin formed following a giant asteroid or comet impact. Water would have flowed from the uplands (to the east) and drained into the low-lying basin, carving river channels as it flowed. The gentle curves-called "meanders" by geomorphologists-imply that this paleoriver carried lots of sediment along with it, depositing it into Hellas. http://photojournal.jpl.nasa.gov/catalog/PIA20815

STS083-302-002 (4-8 April 1997) --- At the MidDeck Glove Box (MGBX), astronaut Donald A. Thomas, mission specialist, prepares to conduct the Internal Flows in Free Drops (IFFD) experiment. The IFFD is meant to study drops of several liquids, including water, water/glycerin and silicon oil. Flows within the drops and shape and stability are studied under varying acoustic pressure. The MGBX is the overall facility that holds experiments on materials that are not approved for study in the open Spacelab environment.

41D-42-023 (30 Aug-5 Sept 1984) --- The Gascoyne River, an intermittent large wash 500 miles north of Perth, Australia, which flows for nearly a thousand miles across the Macadam Plains. The scant water available in this area either is absorbed in the sands and gravel of the watercourse or quickly evaporates. Most water flows beneath the surface, then, giving support to plant root systems and sustaining green vegetation along the watercourses.

This image captured by NASA 2001 Mars Odyssey spacecraft shows a portion of Hebrus Valles. This channel system was formed by liquid flow of either water or lava, or a combination of both. There is a streamlined island in this image and channels at several different elevations. Orbit Number: 61733 Latitude: 17.9819 Longitude: 127.921 Instrument: VIS Captured: 2015-11-13 20:40 http://photojournal.jpl.nasa.gov/catalog/PIA20234

Today's VIS image shows a portion of Granicus Valles. This channel system is located west of Elysium Mons and likely was created by both lava and water flow related to the Elysium Mons volcanic complex. Orbit Number: 61084 Latitude: 28.5697 Longitude: 129.782 Instrument: VIS Captured: 2015-09-21 10:03 http://photojournal.jpl.nasa.gov/catalog/PIA20098