SPACE
Georgia Tech to lead NASA Center on Lunar Research and Exploration
IMAGE: RESEARCH THEMES DEFINING NASA’S CLEVER CENTER WHICH WILL BE LED BY GEORGIA TECH PROFESSOR THOMAS ORLANDO. view more
CREDIT: GEORGIA INSTITUTE OF TECHNOLOGY
Georgia Tech researchers have been selected by NASA to lead a $7.5 million center that will study the lunar environment and the generation and properties of volatiles and dust. The Center for Lunar Environment and Volatile Exploration Research (CLEVER) will be led by Thomas Orlando, professor in the School of Chemistry and Biochemistry.
CLEVER is the successor to Orlando’s pioneering REVEALS (Radiation Effects on Volatiles and Exploration of Asteroids and Lunar Surfaces) center, and both are part of NASA’s Solar System Exploration Research Virtual Institute (SSERVI) program.
REVEALS and CLEVER look ahead to the return of humans to the moon for sustained periods — a key part of NASA’s plan for space exploration in the coming decade. Volatiles such as water, molecular oxygen, methane, and hydrogen are crucial to supporting human activity on the moon. Dust is also important since the space-weathered particles can pose health effects to astronauts and hazards to the technology and hardware.
The interdisciplinary group of researchers supported by CLEVER will study how the solar wind and micrometeorites produce volatiles, research how ice and dust behave in the lunar environment, develop new materials to deal with potential dust buildup, and invent new analysis tools to support the upcoming crewed missions of the Artemis program.
“The resources and knowledge that CLEVER will produce will be useful for the sustainable presence of humans on the moon,” Orlando says. “We have the correct mix of fundamental science and exploration — real, fundamental, ground-truth measurements; very good theory/modeling; and engineering — an easy mix with Georgia Tech and outside partners.”
Orlando adds that CLEVER adopts a unique perspective on the challenges of understanding how to operate on Earth’s moon. “The atomic and molecular view of processes with angstrom distances and femtosecond time scales can help unravel what is happening on planetary spatial scales and geological time frames,” he says. “We can also translate our knowledge into materials, devices, and technology pretty quickly, and this is necessary if we want to help the Artemis astronauts.”
CLEVER includes investigators from Georgia Tech, University of Georgia, the Florida Space Institute, University of Hawaii, Auburn University, Space Sciences Institute, the Johns Hopkins University Applied Physics Laboratory, Lawrence Berkeley National Laboratory, NASA Ames, NASA Kennedy Space Center, and partners in Italy and Germany. In addition to pursuing a blend of fundamental science and mission support, CLEVER will also emphasize the research and career development of students and young investigators, another important goal of the SSERVI system.
Art: Brice Zimmerman, Georgia Institute of Technology
About Georgia Institute of Technology
The Georgia Institute of Technology, or Georgia Tech, is a public research university developing leaders who advance technology and improve the human condition. The Institute offers business, computing, design, engineering, liberal arts, and sciences degrees. Its nearly 44,000 students representing 50 states and 149 countries, study at the main campus in Atlanta, at campuses in France and China, and through distance and online learning. As a leading technological university, Georgia Tech is an engine of economic development for Georgia, the Southeast, and the nation, conducting more than $1 billion in research annually for government, industry, and society.
Academy students blast off to international space competition
WMG Academy for Young Engineers is preparing for lift-off after being named UK national champions in the European Space Agency’s CanSat competition. Having launched themselves to the top spot in the UK, WMG Academy’s Team Phoenix 2 will soon blast off to the European finals.
Inspired by NASA’s Phoenix Mars Lander mission, the young space explorers from Team Phoenix 2 have designed and manufactured a suborbital satellite capable of measuring and collecting temperature and air pressure data whilst looking for signs of life on a planet by sampling surface dust – all contained within the size and shape of a soft-drinks can. Launched to a height of 1,000 feet, the satellite descends, launching an integrated parachute before transmitting data back to the team at the command centre.
As part of the competition, the students, all aged between 14 and 17 years old and studying a combination of maths, science and engineering, have produced designs and prototypes, submitted testing data and launch reports, and presented to a team of experts, setting themselves apart from over 250 other entries and 12 finalists to take the title of UK national champions.
WMG is based at the University of Warwick.
Commenting on the team’s success, WMG Academy Chief Executive, Stewart Tait, said, “Our students are clearly high-flyers with ambitions that are out of this world. We could not be more proud of Oliver, Joshua, Callum, Amneet, Timurs and George who have worked so hard to design an innovative and successful can-sized satellite.
“This year’s CanSat project was launched by Bob Hodge who has been an integral part of WMG Academy since we opened in 2014. Unfortunately, after a long illness, Bob sadly passed away just a few weeks ago and there is no better way to pay tribute to the time and energy Bob invested in the lives of our young engineers than continuing his legacy of inspiring the next generation through projects like CanSat.
“We are looking forward to taking Team Phoenix2 to the European finals to showcase the incredible engineering talent of WMG Academy students on the international stage.”
An X-ray look at the heart of powerful quasars
Peer-Reviewed PublicationIMAGE: ARTIST’S IMPRESSION OF A QUASAR view more
CREDIT: NOIRLAB/NSF/AURA/J. DA SILVA
Researchers have observed the X-ray emission of the most luminous quasar seen in the last 9 billion years of cosmic history, known as SMSS J114447.77-430859.3, or J1144 for short. The new perspective sheds light on the inner workings of quasars and how they interact with their environment. The research is published in Monthly Notices of the Royal Astronomical Society.
Hosted by a galaxy 9.6 billion light years away from the Earth, between the constellations of Centaurus and Hydra, J1144 is extremely powerful, shining 100,000 billion times brighter than the Sun. J1144 is much closer to Earth than other sources of the same luminosity, allowing astronomers to gain insight into the black hole powering the quasar and its surrounding environment. The study was led by Dr Elias Kammoun, a postdoctoral researcher at the Research Institute in Astrophysics and Planetology (IRAP), and Zsofi Igo, a PhD candidate at the Max Planck Institute for Extraterrestrial Physics (MPE).
Quasars are among the brightest and most distant objects in the known universe, powered by the fall of gas into a supermassive black hole. They can be described as active galactic nuclei (AGN) of very high luminosity that emit vast amounts of electromagnetic radiation observable in radio, infrared, visible, ultraviolet and X-ray wavelengths. J1144 was initially observed in visible wavelengths in 2022 by the SkyMapper Southern Survey (SMSS).
For this study, researchers combined observations from several space-based observatories: the eROSITA instrument on board the Spectrum-Roentgen-Gamma (SRG) observatory, the ESA XMM-Newton observatory, NASA’s Nuclear Spectroscopic Telescope Array (NuSTAR), and NASA’s Neil Gehrels Swift observatory.
The team used the data from the four observatories to measure the temperature of the X-rays being emitted from the quasar. They found this temperature to be around 350 million Kelvin, more than 60,000 times the temperature at the surface of the Sun. The team also found that the mass of the black hole at the quasar’s centre is around 10 billion times the mass of the Sun, and the rate at which it is growing to be of the order of 100 solar masses per year.
The X-ray light from this source varied on a time scale of a few days, which is not usually seen in quasars with black holes as large as the one residing in J1144. The typical timescale of variability for a black hole of this size would be on the order of months or even years. The observations also showed that while a portion of the gas is swallowed by the black hole, some gas is ejected in the form of extremely powerful winds, injecting large amounts of energy into the host galaxy.
Dr. Kammoun, lead author of the paper, says “We were very surprised that no prior X-ray observatory has ever observed this source despite its extreme power.”
He adds, “Similar quasars are usually found at much larger distances, so they appear much fainter, and we see them as they were when the Universe was only 2-3 billion years old. J1144 is a very rare source as it is so luminous and much closer to Earth (although still at a huge distance!), giving us a unique glimpse of what such powerful quasars look like.”
“A new monitoring campaign of this source will start in June this year, which may reveal more surprises from this unique source”.
JOURNAL
Monthly Notices of the Royal Astronomical Society
First observed radio waves from a type Ia supernova
IMAGE: ARTIST’S IMPRESSION OF HELIUM-RICH MATERIAL FROM A COMPANION STAR ACCRETING ONTO A WHITE DWARF. BEFORE THE EXPLOSION, A LARGE AMOUNT OF MATERIAL IS STRIPPED FROM THE COMPANION. THE RESEARCH TEAM HOPES TO CLARIFY THE RELATIONSHIP BETWEEN THE EMITTED STRONG RADIO WAVES AND THIS STRIPPED MATERIAL. view more
CREDIT: ADAM MAKARENKO/W. M. KECK OBSERVATORY
For the first time, astronomers have observed radio waves emitted by a Type Ia supernova, a type of explosion originating from a white dwarf star. This provides important clues to understand how white dwarfs explode.
A Type Ia (One-A) supernova is the nuclear explosion of a white dwarf star. This type of supernova is well known; these supernovae are used by astronomers to measure cosmological distances and the expansion of the Universe. But the explosion mechanism of Type Ia supernovae is not well understood. Solitary white dwarfs don’t explode, so it is thought that mass accretion from a neighboring companion star plays a role in triggering the explosion. The accreted mass is the outer layer of the companion star, so it is normally composed mostly of hydrogen, but it was thought that it should also be possible for a white dwarf to accrete helium from a companion star which had lost its outer layer of hydrogen.
As the white dwarf strips matter from its companion star, not all of the material falls onto the white dwarf; some of it forms a cloud of circumstellar material around the binary star system. When a white dwarf explodes in a cloud of circumstellar material, it is expected that the shockwaves from the explosion traveling through the circumstellar material will excite atoms, causing them to emit strong radio waves. However, although many Type Ia supernovae have been observed exploding within a cloud of circumstellar material, so far astronomers had yet to observe radio wave emissions associated with a Type Ia supernova.
An international team of researchers, including members from Stockholm University and the National Astronomical Observatory of Japan, performed detailed observations of a Type Ia supernova which exploded in 2020. They revealed that this supernova was surrounded by circumstellar material consisting mainly of helium, and also succeeded in detecting radio waves from the supernova. Comparing the observed radio wave strength with theoretical models revealed that the progenitor white dwarf star had been accreting material at a rate of about 1/1000 the mass of the Sun every year. This is the first confirmed Type Ia supernova triggered by mass accretion from a companion star with an outer layer consisting primarily of helium.
It is expected that this observation of radio waves from a helium-rich Type Ia supernova will deepen our understanding of the explosion mechanism and the conditions before a Type Ia supernova. Now the team plans to search for radio emissions from other Type Ia supernovae to elucidate the evolution which leads to the explosion.
These results appeared as Kool et al. “A radio-detected Type Ia supernova with helium-rich circumstellar material” in the journal Nature on May 17, 2023.
JOURNAL
Nature
METHOD OF RESEARCH
Observational study
SUBJECT OF RESEARCH
Not applicable
ARTICLE TITLE
A radio-detected type Ia supernova with helium-rich circumstellar material
ARTICLE PUBLICATION DATE
17-May-2023
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