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Arguably, humankind has never been more aware of the jeopardy we and the planet face because of climate change. As world leaders at COP26 work to accelerate action towards reducing greenhouse gas emissions to keep the goal of 1.5°C temperature rise within reach, we bring you a new easy-to-use guide on what ESA is doing to understand and monitor climate change from space – data that are essential for policy-makers.

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      Preparations for Next Moonwalk Simulations Underway (and Underwater)
      The Arctic is captured in this 2010 visualization using data from NASA’s Aqua satellite. A new study quantifies how climate-related processes, including the melting of ice sheets and glaciers, are driving polar motion. Another study looks at how polar meltwater is speeding the lengthening of Earth’s day.NASA’s Scientific Visualization Studio Researchers used more than 120 years of data to decipher how melting ice, dwindling groundwater, and rising seas are nudging the planet’s spin axis and lengthening days.
      Days on Earth are growing slightly longer, and that change is accelerating. The reason is connected to the same mechanisms that also have caused the planet’s axis to meander by about 30 feet (10 meters) in the past 120 years. The findings come from two recent NASA-funded studies focused on how the climate-related redistribution of ice and water has affected Earth’s rotation.
      This redistribution occurs when ice sheets and glaciers melt more than they grow from snowfall and when aquifers lose more groundwater than precipitation replenishes. These resulting shifts in mass cause the planet to wobble as it spins and its axis to shift location — a phenomenon called polar motion. They also cause Earth’s rotation to slow, measured by the lengthening of the day. Both have been recorded since 1900.
      To view this video please enable JavaScript, and consider upgrading to a web browser that supports HTML5 video
      The animation, exaggerated for clarity, illustrates how Earth’s rotation wobbles as the location of its spin axis, shown in orange, moves away from its geographic axis, which is shown in blue and represents the imaginary line between the planet’s geographic North and South poles.NASA’s Scientific Visualization Studio Analyzing polar motion across 12 decades, scientists attributed nearly all of the periodic oscillations in the axis’ position to changes in groundwater, ice sheets, glaciers, and sea levels. According to a paper published recently in Nature Geoscience, the mass variations during the 20th century mostly resulted from natural climate cycles.
      The same researchers teamed on a subsequent study that focused on day length. They found that, since 2000, days have been getting longer by about 1.33 milliseconds per 100 years, a faster pace than at any point in the prior century. The cause: the accelerated melting of glaciers and the Antarctic and Greenland ice sheets due to human-caused greenhouse emissions. Their results were published July 15 in Proceedings of the National Academy of Sciences.
      “The common thread between the two papers is that climate-related changes on Earth’s surface, whether human-caused or not, are strong drivers of the changes we’re seeing in the planet’s rotation,” said Surendra Adhikari, a co-author of both papers and a geophysicist at NASA’s Jet Propulsion Laboratory in Southern California.
      To view this video please enable JavaScript, and consider upgrading to a web browser that supports HTML5 video
      The location of Earth’s spin axis moved about 30 feet (10 meters) between 1900 and 2023, as shown in this animation. A recent study found that about 90% of the periodic oscillations in polar motion could be explained by melting ice sheets and glaciers, diminishing groundwater, and sea level rise.NASA/JPL-Caltech Decades of Polar Motion
      In the earliest days, scientists tracked polar motion by measuring the apparent movement of stars. They later switched to very long baseline interferometry, which analyzes radio signals from quasars, or satellite laser ranging, which points lasers at satellites.
      Researchers have long surmised that polar motion results from a combination of processes in Earth’s interior and at the surface. Less clear was how much each process shifts the axis and what kind of effect each exerts — whether cyclical movements that repeat in periods from weeks to decades, or sustained drift over the course of centuries or millennia.
      For their paper, researchers used machine-learning algorithms to dissect the 120-year record. They found that 90% of recurring fluctuations between 1900 and 2018 could be explained by changes in groundwater, ice sheets, glaciers, and sea level. The remainder mostly resulted from Earth’s interior dynamics, like the wobble from the tilt of the inner core with respect to the bulk of the planet.
      The patterns of polar motion linked to surface mass shifts repeated a few times about every 25 years during the 20th century, suggesting to the researchers that they were largely due to natural climate variations. Past papers have drawn connections between more recent polar motion and human activities, including one authored by Adhikari that attributed a sudden eastward drift of the axis (starting around 2000) to faster melting of the Greenland and Antarctic ice sheets and groundwater depletion in Eurasia.
      That research focused on the past two decades, during which groundwater and ice mass loss as well as sea level rise — all measured via satellites — have had strong connections to human-caused climate change.
      “It’s true to a certain degree” that human activities factor into polar motion, said Mostafa Kiani Shahvandi, lead author of both papers and a doctoral student at the Swiss university ETH Zurich. “But there are natural modes in the climate system that have the main effect on polar motion oscillations.”
      Longer Days
      For the second paper, the authors used satellite observations of mass change from the GRACE mission (short for Gravity Recovery and Climate Experiment) and its follow-on GRACE-FO, as well as previous mass-balance studies that analyzed the contributions of changes in groundwater, ice sheets, and glaciers to sea level rise in the 20th century to reconstruct changes in the length of days due to those factors from 1900 to 2018.
      Scientists have known through historical eclipse records that length of day has been growing for millennia. While almost imperceptible to humans, the lag must be accounted for because many modern technologies, including GPS, rely on precise timekeeping.
      In recent decades, the faster melting of ice sheets has shifted mass from the poles toward the equatorial ocean. This flattening causes Earth to decelerate and the day to lengthen, similar to when an ice skater lowers and spreads their arms to slow a spin.
      The authors noticed an uptick just after 2000 in how fast the day was lengthening, a change closely correlated with independent observations of the flattening. For the period from 2000 to 2018, the rate of length-of-day increase due to movement of ice and groundwater was 1.33 milliseconds per century — faster than at any period in the prior 100 years, when it varied from 0.3 to 1.0 milliseconds per century.
      The lengthening due to ice and groundwater changes could decelerate by 2100 under a climate scenario of severely reduced emissions, the researchers note. (Even if emissions were to stop today, previously released gases — particularly carbon dioxide — would linger for decades longer.)
      If emissions continue to rise, lengthening of day from climate change could reach as high as 2.62 milliseconds per century, overtaking the effect of the Moon’s pull on tides, which has been increasing Earth’s length of day by 2.4 milliseconds per century, on average. Called lunar tidal friction, the effect has been the primary cause of Earth’s day-length increase for billions for years.
      “In barely 100 years, human beings have altered the climate system to such a degree that we’re seeing the impact on the very way the planet spins,” Adhikari said.
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      Earth Observer Earth Home Earth Observer Home Editor’s Corner Feature Articles Meeting Summaries News Science in the News Calendars In Memoriam More Archives 18 min read
      Summary of the 2023 Sun – Climate Symposium
      Introduction
      Observations of the Sun and Earth from space continue to revolutionize our view and understanding of how solar variability and other natural and anthropogenic forcings impact Earth’s atmosphere and climate. For more than four decades (spanning four 11-year solar cycles and now well into a fifth), the total and spectral solar irradiance and global terrestrial atmosphere and surface have been observed continuously, providing an unprecedented, high-quality time series of data for Sun–climate studies, such as the Total Solar Irradiance (TSI) composite record – see Figure 1.
      Figure 1. The Total Solar Irradiance (TSI) composite record spans almost 5 decades and includes measurements from 13 different instruments (9 NASA and 4 international). Figure credit: Greg Kopp, Laboratory for Atmospheric and Space Physics (LASP)/University of Colorado (UC). Sun–Climate Symposia, originally called SOlar Radiation and Climate Experiment (SORCE) Science Team Meetings, have been held at a regular cadence since 1999 – before the launch of SORCE in 2003. These meetings provide an opportunity for experts from across the solar, Earth atmosphere, climate change, stellar, and planetary communities to present and discuss their research results about solar variability, climate influences and the Earth-climate system, solar and stellar variability comparative studies, and stellar impacts on exoplanets.
      The latest iteration was the eighteenth in the series and occurred in October 2023. (As an example of a previous symposium, see Summary of the 2022 Sun–Climate Symposium, in the January–February 2023 issue of The Earth Observer [Volume 35, Issue 1, pp. 18–27]). The 2023 Sun–Climate Symposium took place October 17­–20 in Flagstaff, AZ – with a focus topic of “Solar and Stellar Variability and its Impacts on Earth and Exoplanets.” The Sun–Climate Research Center – a joint venture between NASA’s Goddard Space Flight Center (GSFC) and the Laboratory for Atmospheric and Space Physics (LASP) at the University of Colorado (UC) with the Lowell Observatory hosting the meeting. The in-person meeting had 75 attendees – including 7 international participants – with diverse backgrounds covering a wide range of climate change and solar-stellar variability research topics – see Photo.
      Photo. Attendees at the 2023 Sun–Climate Symposium in Flagstaff, AZ. Photo credit: Kelly Boden/LASP Update on NASA’s Current and Planned TSIS Missions
      The current NASA solar irradiance mission, the Total and Spectral Solar Irradiance Sensor (TSIS-1), marks a significant advance in our ability to measure the Sun’s energy input to Earth across various wavelengths. Following in the footsteps of its predecessors, most notably SORCE, TSIS-1 contributes to the continuous time series of solar energy data dating back to 1978 – see Figure 1. The two instruments on TSIS-1 improve upon those on previous missions, enabling scientists to study the Sun’s natural influence on Earth’s ozone layer, atmospheric circulation, clouds, and ecosystems. These observations are essential for a scientific understanding of the effects of solar variability on the Earth system. 
      TSIS-1 launched to the International Space Station (ISS) in December 2017 and is deployed on the Station’s EXpedite the PRocessing of Experiments to Space Station (ExPRESS) Logistics Carrier–3 (ELC-3). Its payload includes the Total Irradiance Monitor (TIM) for observing the TSI and the Spectral Irradiance Monitor (SIM) for measuring the Solar Spectral Irradiance (SSI) – see comparison in Figure 2. The mission completed its five-year prime science mission in March 2023. SIM measures from 200–2400 nm with variable spectral resolution ranging from about 1 nm in the near ultraviolet (NUV) to about 10 nm in the near infrared (NIR). TSIS-1 has been extended by at least three more years as part of the Earth Sciences Senior Review process.
      TSIS-2 is intended as the follow-on to TSIS-1. The mission is currently in development at LASP and GSFC with a planned launch around mid 2025. The TSIS-2 payload is nearly identical to that of TSIS-1, except that the payload will ride on a free-flying spacecraft rather than be mounted on a solar pointing platform on the ISS. NASA hopes to achieve 1–2 years of overlap between TSIS-1 and TSIS-2. Achieving such measurement overlap between missions is crucial to the continuity of the long-term records of the TSI and SSI without interruption and improving the solar irradiance composite.
      In addition to the current solar irradiance mission and its planned predecessor, NASA is always looking ahead to plan for the inevitable next solar irradiance mission. Two recent LASP CubeSat missions – called Compact SIM (CSIM) and Compact TIM (CTIM) – have tested miniaturized versions of the SIM and TIM instruments, respectively. Both CSIM and CTIM have performed extremely well in space – with measurements that correlate well with the larger instruments – and are being considered as continuity options for the SSI and TSI measurements. Based on the success of CSIM and CTIM, LASP has developed a concept study report about the Compact-TSIS (CTSIS) as a series of small satellites viable for a future TSIS-3 mission.
      Figure 2. The Solar Spectral Irradiance (SSI) variability from TSIS-1 Spectral Irradiance Monitor (SIM) is compared to the Total Solar Irradiance (TSI) variability from TSIS-1 Total Irradiance Monitor (TIM). The left panel shows the SIM SSI integrated over its wavelength range of 200–2400 nm, which is in excellent agreement with the TSI variability during the rising phase of solar cycle 25. The right panels show comparison of SSI variability at individual wavelengths to the TSI variability, revealing linear relationships with ultraviolet variability larger than TSI variability, visible variability similar to TSI variability, and near infrared variability smaller than TSI variability. Figure credit: Erik Richard/LASP Meeting Overview
      After an opening plenary presentation in which Erik Richard [LASP] covered the information on TSIS-1, TSIS-2, CSIM, and CTIM presented in the previous section on “NASA’s Current and Planned Solar Irradiance Missions,” the remainder of the four-day meeting was divided into five science sessions each with oral presentations, and a poster session featuring 23 contributions.
      The five session topics were:
      Solar and Stellar Activity Cycles Impacts of Stellar Variability on Planetary Atmospheres Evidence of Centennial and Longer-term Variability in Climate Change Evidence of Short-term Variability in Climate Change Trending of Solar Variability and Climate Change for Solar Cycle 25 (present and future) There was also a banquet held on the final evening of the meeting (October 19) with special presentations focusing on the water drainage system and archaeology of the nearby Grand Canyon – see Sun-Climate Symposium Banquet Special Presentation on the Grand Canyon National Park.
      The remainder of this report summarizes highlights from each of the science sections. To learn more, the reader is referred to the full presentations from the 2023 Sun–Climate Symposium, which can be found on the Symposium website by clicking on individual presentation titles in the Agenda tab.
      Session 1: Solar and Stellar Activity Cycles
      Sun-like stars (and solar analogs, solar twins) provide a range of estimates for how the Sun’s evolution may affect its solar magnetic cycle variability. Recent astrophysics missions (e.g., NASA’s Kepler mission) have added thousands of Sun-like stars to study, compared to just a few dozen from a couple decades ago when questions remained if the Sun is a normal G star or not.
      Tom Ayres [UC Center for Astrophysics and Space Astronomy (CASA)] gave the session’s keynote presentation on Sun-like stars. He pointed out that the new far ultraviolet (FUV) and X-ray stellar observations have been used to clarify that our Sun is a normal G-type dwarf star with low activity relative to most other G-type dwarf stars.
      Travis Metcalfe [White Dwarf Research Corporation (WDRC)] discussed the recent progress in modeling of the physical processes that generate a star’s magnetic field – or stellar dynamo. He explained how the presence of stellar wind can slow down a star’s rotation, which in turn lengthens the period of the magnetic cycle. He related those expectations to the Sun and to the thousands of Sun-like stars observed by Kepler.
      Continuing on the topic of solar dynamo, Lisa Upton [Space Systems Research Corporation (SSRC)] and Greg Kopp [LASP] discussed their recent findings using a solar surface magnetic flux transport model, which they can use to reconstruct an estimated TSI record back in time to the anomalously low activity during the Maunder Minimum in the 1600s. Dan Lubin [University of California San Diego (UCSD)] described efforts to identify grand-minimum stars – which exhibit characteristics similar to our Sun during the Maunder Minimum. Using Hamilton Echelle Spectrograph observations, they have identified about two dozen candidate grand-minimum stars.
      In other presentations and posters offered during this session, Adam Kowalski [LASP]) discussed stellar and solar flare physics and revealed that the most energetic electrons generated during a flare are ten times more than previously thought, while Moira Jardine [University of St. Andrews, Scotland]) discussed the related subject of space weather on the Sun and stars and how the coronal extent was likely much larger for the younger Sun. Three presenters – Debi Choudhary [California State University, Northridge], Garrett Zills [Augusta University], and Serena Criscuoli [National Solar Observatory] –discussed how solar emission line variability from both line intensity and line width are good indicators of magnetic activity on the Sun and thus relevant for studies of Sun-like star variability. Andres Munoz-Jaramillo [Southwest Research Institute (SWRI)] highlighted the importance of archiving large datasets showing the Harvard dataverse as an example. Juan Arjona [LASP] discussed the solar magnetic field observations made using the Max Planck Institute for Solar System Research’s GREGOR solar telescope.
      Session 2: Impacts of Stellar Variability on Planetary Atmospheres
      Presenters in this session focused on how the stellar variability can impact exoplanet evolution and climate. By analyzing data from NASA’s Kepler mission, scientists have discovered numerous Earth-like planets orbiting other stars – or exoplanets, which has enabled comparative studies between planets in our Solar System and exoplanets.
      Aline Vidotto [University of Leiden, Netherlands] gave this session’s keynote presentation in which he discussed the impact of stellar winds on exoplanets. In general, younger stars rotate faster and thus have more stellar variability. The evolution of the exoplanet’s atmosphere is dependent on its star’s variability and also modulated by the exoplanet’s own magnetic field. Robin Ramstad [LASP] further clarified a planetary magnetic field’s influences on atmospheric evolution for planets in our solar system.
      Vladimir Airapetian [GSFC] presented an overview of how laboratory measurements used to simulate pre-biosignatures – characteristics that precede those elements, molecules, or substances that would indicate past or present life – could be created in an exoplanet atmosphere by highly energetic particles and X-rays from stars with super flares, very large-scale magnetic eruptions on a star that can be thousands of times brighter than a typical solar flare. While the probability of a super flare event is low for our Sun (perhaps 1 every 400 years), super flares are routinely observed on more active stars.
      The stellar flares and the spectral distribution of the flare’s released energy can have large impacts on exoplanet’s atmospheres. Laura Amaral [Arizona State University] presented on the super-flare influences on the habitable zone of exoplanets and explained how the flare’s significantly enhanced X-ray emissions would greatly accelerate water escape from the exoplanet’s atmosphere. Ward Howard [ UC CASA] showed that exoplanet transits can also provide information about starspots (akin to the dark sunspots on the Sun) when a transit event happens to occult a starspot – see Figure 3. Ward also explained the importance of observing the transit events at multiple wavelengths, referred to as transit spectroscopy, to understand the physical characteristics of the starspots. Yuta Notsu [LASP] compared the energetics observed in many different stars using X-ray and far ultraviolet (FUV) observations to estimate stellar magnetic field strengths, which in turn can be used to estimate the stellar extreme ultraviolet (EUV) spectra. Those results provide new information on how the stellar spectra could evolve during the lifetime of Sun-like stars, and how those spectral changes can affect the atmospheric escape rates on their exoplanets.  
      Nina-Elisabeth Nemec [University of Göttingen, Germany] described how Kepler observations of exoplanets rely on tracking their transits across its host star’s disk. She explained some of the challenges that arise with analyzing such transits when there are large starspots present. 
      Figure 3. Illustration of an exoplanet transit that will occult a starspot. The transit light curve can provide information about the size of the starspot, and transit observations at multiple wavelengths can reveal physical parameters, such as temperature, of the starspot. Figure credit: Ward Howard, CASA/University of Colorado Session 3: Evidence of Centennial and Longer-term Variability in Climate Change
      Venkatachalam “Ram” Ramaswamy [National Oceanic and Atmospheric Administration’s (NOAA) Geophysical Fluid Dynamics Laboratory (GFDL)] gave the keynote for this session in which he discussed Earth’s variable climate change over the past two centuries. He explained in detail Earth’s energy budget and energy imbalance, which leads to less land and sea ice, warmer temperatures at the surface and in the atmosphere and ocean, and more extreme weather. These weather changes have different regional impacts, such as more floods in some regions and more drought in different regions – see Figure 4. 
      Figure 4. The rainfall amount has shifted over the past fifty years (red is less and blue is more) with strong regional impacts on droughts and floods. Figure credit: Ram Ramaswamy/NOAA/GFDL Bibhuti Kumar Jha [SWRI], Bernhard Hofer [Max Planck Institute for Solar System Research, Germany], and Serena Criscuoli [National Solar Observatory] discussed long-term solar measurements from the Kodaikanal Solar Observatory and showed that the chromospheric plages (Ca K images) have 1.6% faster solar rotation rate than sunspots (white light images). Timothy Jull [University of Arizona (UA)], Fusa Miyake [Nagoya University, Japan], Georg Fueulner [Potsdam Institute for Climate Impact Research, Germany], and Dan Lubin discussed the impact that solar influences (i.e., solar flares, solar energetic particles) have had on Earth’s climate over hundreds of years through their impact on phenomena such as the natural distribution of carbon dioxide in the atmosphere and fluctuations in the North Atlantic Oscillation.  
      Hisashi Hayawawa [Nagoya University] and Kalevi Mursula [University of Oulu, Finland] discussed the influence that ever-changing sunspots and magnetic fields on the Sun are having on climate – with a focus on the Maunder Minimum period. Irina Panyushkina [UA] and Timothy Jull presented tree ring radioisotope information as it relates to climate change trends as well as long-term, solar variability trends. According to Lubin, if a reduction in solar input similar to what happened during the Maunder Minimum would happen today, the resulting reduction in temperature would be muted due to the higher concentration of greenhouse gases (GHG) in the atmosphere.
      Session 4: Evidence of Short-term Variability in Climate Change
      Session 4 focused on discussions that examined shorter-term variations of solar irradiance and climate change. Bill Collins [Lawrence Berkeley National Laboratory (LBNL)] started off the session with a presentation on Earth albedo asymmetry across the hemispheres from Nimbus-7 observations, and then showed some important differences when looking at the Clouds and the Earth’s Radiant Energy System (CERES) record – shown in Figure 5. Lon Hood [UA] discussed the changes in atmospheric circulation patterns which might be the consequence of Arctic sea ice loss increasing the sea level pressure over northern Eurasia. Alexi Lyapustin [GSFC] described how higher temperatures are causing an extension of the wildfire season in the Northern hemisphere by 1–3 months.
      Figure 5. The albedo difference between the visible and near-infrared bands are shown for the southern hemisphere (red line) and the northern hemisphere (blue lines) for CERES [left] and Nimbus 7 [right]. The southern hemisphere albedo difference is higher than the northern hemisphere albedo difference, both for the 1980s as measured by Nimbus-7 and for the recent two decades as measured by CERES. These hemispheric differences are related mostly to differences in cloud coverage. The seasonal effect on the albedo difference values is about 2%, but the changes from 1980s to 2010s appear to be about 10%. Figure credit: Bill Collins/Lawrence Berkeley National Laboratory Jae Lee [GSFC/University of Maryland, Baltimore County] discussed changes in the occurrence and intensity of the polar mesosphere clouds (PMCs), showing high sensitivity to mesospheric temperature and water, and fewer PMCs for this solar cycle. In addition, some presenters discussed naturally driven climate changes. Luiz Millan [JPL], whose research has found that the water-laden plume from the Hunga-Tonga-Hunga-Ha’apai (HT-HH) volcano eruption in January 2022 has had a warming effect on the atmosphere as well as the more typical cooling effect at the surface from the volcanic aerosols. In another presentation, Jerry Raedar [University of New Hampshire, Space Science Center] showed results from his work indicating about 5% reductions in temperature and pressure following major solar particle storms, but noted differences in dependence between global and regional effects.
      Session 5: Trending of Solar Variability and Climate Change for Solar Cycle 25 (present and future)
      Session 5 focused on trends during Solar cycle 25 (SC-25), which generated lively discussions about predictions. It appears the SC-25 maximum sunspot number could be about 15% higher than the original SC-25 maximum predictions. Those differences between the sunspot observations and this prediction may be related to the timing of SC-25 ramp up. Lisa Upton started off Session 5 by presenting both the original and latest predictions from the NASA–NOAA SC-25 Prediction Panel. Her assessment of the Sun’s polar magnetic fields and different phasing of magnetic fields over the Sun’s north and south poles suggests that the SC-25 maximum will be larger than the prediction – see Figure 6.
      The next several speakers – Matt DeLand [Science Systems and Applicatons Inc. (SSAI)], Sergey Marchenko [SSAI], Dave Harber [LASP], Tom Woods [LASP], and Odele Coddington [LASP] – showed a variety of TSI and SSI (NUV, visible, and NIR) variability observations during SC-25. The group consensus was that the difference between the SC-24 and SC-25 maxima may be due to the slightly higher solar activity during SC-25 as compared to the time of the SC-24 maximum – which was an anomalously low cycle. The presenters all agreed that SC-25 maximum may not have been reached yet (and SC-25 maximum may not have occurred yet in 2024).
      Figure 6. The sunspot number progression (black) during solar cycle 25 is higher than predicted (red). The original NASA–NOAA panel prediction was for a peak sunspot number of 115 in 2025. Lisa Upton’s updated prediction is for a sunspot number peak of 134 in late 2024. Figure credit: NOAA Space Weather Prediction Center On the climate change side, Don Wuebbles [University of Illinois, Urbana-Champaign] provided a thorough overview of climate change science showing that: the largest impacts result from the activities of humans, land is warming faster than the oceans, the Arctic is warming two times faster than rest of the world, and 2023 was the hottest year on record with an unprecedented number of severe weather events.
      There were several presentations about the solar irradiance observations. Leah Ding [American University] presented new analysis techniques using machine learning with Solar Dynamics Observatory (SDO) solar images to study irradiance variability. Steve Penton [LASP] discussed new SIM algorithm improvements for TSIS-1 SIM data product accuracy. Margit Haberreiter [Physikalisch-Meteorologisches Observatorium Davos (PMOD), Switzerland] discussed new TSI observations from the Compact Lightweight Absolute Radiometer (CLARA) on the Norwegian NorSat-1 microsatellite. Marty Snow [South African National Space Agency] discussed a new TSI-proxy from the visible light (green filter) Solar Position Sensor (SPS) flown on the NOAA Geostationary Operational Environmental Satellites (GOES-R). (The first of four satellites in the GOES-R series launched in 2016 (GOES-16) followed by GOES-17 and GOES-18 in 2018 and 2022 respectively. The final satellite in the series – GOES-U – launched June 25, 2024 will become GOES-19 after checkout is complete.)
      Peter Pilewskie [LASP] discussed future missions, focusing on the Libera mission for radiative energy budget, on which he is Principal Investigator. Selected as the first Earth Venture Continuity mission (EVC-1), Libera will record how much energy leaves our planet’s atmosphere on a day-by-day basis providing crucial information about how Earth’s climate is evolving. In Roman mythology, Libera was Ceres’ daughter. The mission name is thus fitting as Libera will act as a follow-on mission to maintain the decades long data record of observation from NASA’s suite of CERES instruments. Figure 7 shows the CERES climate data record trends over the past 20 years.
      Figure 7. The CERES Earth Radiation Budget (ERB) climate data record shows a positive trend for the absorbed solar radiation [left] and the net radiation [right] and a small negative trend for the emitted terrestrial radiation [middle]. Figure credit: Peter Pilewskie/adapted from a 2021 paper in Geophysical Research Letters Susan Breon [GSFC] discussed the plans for and status of TSIS-2 , and Tom Patton [LASP] discussed CTSIS as an option for TSIS-3 – both of these topics were discussed earlier in this article in the section on “NASA’s Current and Planned Solar Irradiance Missions.”
      Angie Cookson [California State University, San Fernando Observatory (SFO)] shared information about the SFO’s 50-year history, and how analyses of solar image observations taken at SFO are used to derive important indicators of solar irradiance variability – see Figure 8.
      Figure 8. The San Fernando Observatory (SFO) [left] has been making visible [middle] and near ultraviolet (NUV) [right] solar images from the ground for more than 50 years. Those solar images have been useful for understanding the sources of solar irradiance variability. Figure credit: Angie Cookson/SFO Sun-Climate Symposium Banquet Special Presentation on the Grand Canyon National Park
      At the Thursday evening banquet, two speakers – Mark Nebel and Anne Millar – from the National Park Service (NPS) presented some of their geological research on the nearby Grand Canyon. Nebel discussed the water drainage systems surrounding the Grand Canyon while Millar described the many different fossils that have been found in the surrounding rocks. Nebel explained how  the Grand Canyon’s water drainage system into the Colorado River is complex and has evolved over the past few decades – see map and photo below. Millar brought several samples of the plant and insect fossils found in the Grand Canyon to share with banquet participants. Those fossils ranged in time from the Bright Angel Formation ocean period 500 million years ago to the Hermit Formation period 285 million years ago – when the Grand Canyon was semi-arid land with slow-moving rivers.
      Map and photo credit: Mark Nebel/NPS Conclusion
      Altogether, 80 presentations during the 2023 Sun–Climate Symposium spread across 6 sessions about solar analogs, exoplanets, long-term climate change, short-term climate change, and solar/climate recent trending. The multidisciplinary group of scientists attending made for another exciting conference for learning more about the TSIS solar irradiance observations. Sun–Climate recent results have improved perception of our Sun’s variability relative to many other Sun-like stars, solar impact on Earth and other planets and similar type impacts of stellar variability on exoplanets, and better characterization of anthropogenic climate drivers (e.g., increases in GHG) and natural climate drivers (Sun and volcanoes).
      The next Sun–Climate Symposium will be held in spring 2025 with a potential focus on polar climate records, including polar ice trends and long-term solar variabilities derived from ice-core samples. Readers who may be interested in participating in the 2025 science organizing committee should contact Tom Woods and/or Dong Wu [GSFC].
      Acknowledgments
      The three co-authors were all part of the Science Organizing Committee for this meeting and wish to acknowledge the other members for their work in planning for and participating in another successful Sun–Climate Symposium. They include: Odele Coddington, Greg Kopp, and Ed Thiemann [all at LASP]; Jae Lee, Doug Rabin, and Dong Wu [all at GSFC]; Jeff Hall, Joe Llama, and Tyler Ryburn [all at Lowell Observatory]; Dan Lubin [UCSD’s Scripps Institution of Oceanography (SIO)]; and Tom Stone [U.S. Geological Survey’s Astrogeology Science Center]. The authors and other symposium participants are also deeply grateful to Kelly Boden [LASP] for organizing the logistics and management of the conference, and to the Lowell Observatory, the Drury Inn conference center staff, and the LASP data system engineers for their excellent support in hosting this event.
      Tom Woods
      University of Colorado, Laboratory for Atmospheric and Space Research
      tom.woods@lasp.colorado.edu
      Peter Pilewskie
      University of Colorado, Laboratory for Atmospheric and Space Research
      peter.pilewskie@lasp.colorado.edu
      Erik Richard
      University of Colorado, Laboratory for Atmospheric and Space Research
      erik.richard@lasp.colorado.edu
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      Last Updated Jul 18, 2024 Related Terms
      Earth Science Uncategorized View the full article
    • By Space Force
      Col. Patrick took command of SPACEFOR-KOR from his previous assignment at Ramstein Air Base, Germany, he is a career space operations officer, with command experience at the squadron level and joint experience in both Germany and Belgium.

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    • By NASA
      7 Min Read Spectral Energies is a NASA SBIR/STTR-Funded Tech that Could Change the Way We Fly
      City scape of New York City at sunrise with multiple airplanes and other flying vehicles. Credits: NASA SBIR/STTR Editor Note: Article written by Nicholas Mercurio
      With $20 million in commercial sales and $15 million in sales to government agencies, minority-owned small business Spectral Energies, based in Beavercreek, Ohio, has found a customer base for its pulse-burst laser systems. NASA has played a significant role in developing the technology through the Small Business Innovation Research (SBIR) / Small Business Technology Transfer (STTR) program. With wide-ranging applications including metrology to support commercial aircraft certification, as well as material processing, this technology could pave the way for new forms of passenger aircraft.
      The High Cost of Aircraft Certification
      Did you know that the Boeing 737 first entered service in 1968? Yet there’s a good chance that, if you’ve flown recently, it was on a Boeing 737. That’s due in large part to the cost of certifying new airplanes, which can range in the hundreds of millions of dollars. One place to look for cost savings is the testing process.
      When testing a new design for a space vehicle or commercial aircraft, researchers use wind tunnels to simulate flight conditions. The new aircraft or aircraft component—such as a new wing design—is built, put inside the wind tunnel, and evaluated.
      NASA has long sought to develop robust modeling and prediction software to significantly reduce the need for wind tunnel testing and expensive flight testing. Such software would allow initial analysis to be done on a computer model to identify performance improvement opportunities and iterate on designs, saving the actual manufacturing and its associated costs for a design much closer to being final. Innovations in laser measurement systems could finally bring this goal within reach.
      The Limitations of Traditional Lasers and Early Pulse-Burst Laser Systems
      Entering into use in the 1980s and still widely used today, traditional commercial laser systems operate at 10 Hz, meaning they can fire 10 times per second into the air moving around an aircraft in a wind tunnel. This essentially provides a “photograph” of the air flow at that moment.
      But a tenth of a second is a long time, especially when NASA wind tunnels can test vehicles at up to ten times the speed of sound. In a tenth of a second, the pocket of air from the previous image has long since moved on, meaning the second image is capturing something completely different than the first and crucial data is lost.  
      Why is this data crucial? Because when an aircraft has stalled, it’s the air flow—how the air moves over, under, and around the aircraft—that matters. This air flow changes rapidly in time, leading to effects like stall and buffet; measurement techniques need to be able to capture these rapid changes. Without a complete, data-backed understanding of air flow moment to moment, efforts to develop accurate modeling software have stalled.
      In the late 1990s, pulse-burst laser systems came onto the scene and delivered a dramatic increase in measurement speed. These systems—developed in part with support from the NASA SBIR program—went from producing a set of photograph-like images to delivering a movie-like sequence of data. However, these early systems were difficult to transport and operate, significantly limiting their use.
      NASA SBIR/STTR phasesCredits: NASA SBIR/STTR Enhancing Usability with Air Force SBIR Funding
      By providing funding to develop early-stage technologies, the NASA SBIR/STTR program helps de-risk and develop ideas, maturing them to the point where others can continue innovating. More than a decade after helping to fund some of the earliest pulse-burst laser systems, NASA awarded Phase I SBIR funding to Spectral Energies in 2009 for further advancement of the technology.
      The firm went on to receive Phase II and Phase III SBIR funding from the U.S. Air Force, leveraging these awards to create a commercial pulse-burst laser system that was smaller, easier to transport, more resilient and reliable, and simpler to operate due to significant software advancements. Air Force funding also enabled Spectral Energies to demonstrate several new applications of the system in combustion environments.
      With this foundational work in place, the technology was ready for further innovation to help NASA pursue its long-held goal of more effective air flow measurement and modeling.
      Spectral Energies work with the NASA SBIR/STTR program
      Spectral Energies resumed its work with the NASA SBIR/STTR program in 2014 with multiple Phase I awards. Through continuing program awards, including three Phase II Extended (II-E) and three Phase III contracts, the firm added new capabilities to its pulse-burst laser system, such as high-speed two-color thermometry, demonstrated in 2020.
      Previously, two-color thermometry was typically done at 10 Hz speeds with two lasers and two cameras. Spectral Energies worked with NASA to develop this capability at high-speed using their single-laser, single-camera system, thereby enabling three- and four-dimensional (i.e., three spatial coordinates and time) temperature measurement of chemical flows, a critical capability when designing new chemical propulsion systems.
      Further collaboration with NASA yielded additional capabilities in high-speed picosecond velocimetry and two-dimensional ultraviolet spectroscopy and imaging. Adding these measurement techniques to its technology allowed Spectral Energies to make commercial inroads into hypersonic wind tunnel testing, material processing, and defense applications. Rather than modifying the pulse-burst laser system to deliver these capabilities, each enhancement took the form of an add-on that could be attached to the system, similar to how you can add apps to your smart phone or attach a new lens to your camera. These NASA SBIR-funded add-ons have increased the return on investment (ROI) for each of Spectral Energies’ customers across federal agencies, research universities, and commercial companies.
      Growing a Small Business
      For small businesses, the hunger to do more is often quelled by the reality of limited resources. As a result, necessity is often the biggest driver of decision-making: What do we need to do today to keep our doors open tomorrow? Funding from the NASA SBIR/STTR program allowed Spectral Energies to move into a different mindset and tap into their creative drive.
      “Through the NASA program, we started diversifying in hypersonic test facilities from subsonic combustion facilities,” said Dr. Sukesh Roy, CEO of Spectral Energies, “and that opened many doors for the application of this laser, from detonation to directed energies. Without the funding from NASA, it would have been impossible for us to push for versatile technological enhancements that significantly broadened the application field.” Moving into the research and development of new applications allowed the company to widen its focus and ultimately find a larger customer base.
      Spectral Energies’ continued work with the NASA SBIR/STTR program has helped the company further grow and succeed. By providing entry into new industries and new capabilities for existing customers, the add-on technologies developed with NASA SBIR-funding have generated significant commercial revenue for the small business. Additionally, these developments have opened the door for new funding opportunities with the Air Force, Navy, Army, and Missile Defense Agency.
      Without the funding from NASA, it would have been impossible for us to push for versatile technological enhancements that significantly broadened the application field.
      Dr. Sukesh Roy
      CEO of Spectral Energies
      Providing Benefit to NASA and Beyond
      Dr. Paul Danehy, Senior Technologist for Advanced Measurement Systems at NASA’s Langley Research Center, has worked with Spectral Energies on a number of projects through the program. According to Dr. Danehy, not only did NASA SBIR funding aid the company’s technology growth, program funding also made it possible for NASA researchers to make use of this technology.
      As Dr. Danehy explains, SBIR/STTR Post Phase II funding vehicles like Phase II-E and Phase III allow other programs within NASA to pool money together, then receive matching funds from the SBIR/STTR program. This matching funding increases the purchasing power of other NASA programs and has allowed the agency to acquire two of Spectral Energies’ pulse-burst laser systems, complete with add-ons.
      Agency researchers are using these pulse-burst laser systems to obtain unique quantitative flow field measurements that will allow them to refine software codes to accurately design and evaluate new aerospace vehicles. In time, these software codes could cut hundreds of millions of dollars from the certification of commercial aircraft, allowing new planes to be developed and made available to passengers faster and cheaper.
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    • By NASA
      NASA Science Live: Climate Edition - Rising Heat
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