HUN-REN ATOMKI
Space Chemistry
Research Group
Astrophysics
Astrochemistry
Materials Science for Space
Mission
Humanity is entering an exciting era of space exploration and exploitation in which we will conduct an exploration programme of the planets and moons in and beyond our own Solar System, as well as establishin a permanent presence of humans in space, such as on lunar bases or platforms in Earth and lunar orbit.
Compared to the terrestrial surface, space represents a hostile environment characterised by a wide range of temperatures, extreme vacuum conditions, and an active radiation environment; all of which influence the physical processes that occur there. This requires a new understanding (and, often, reinterpretation) of many basic physical phenomena, which to date have been assessed and defined purely in a terrestrial context.
The mission of the HUN-REN ATOMKI Space Chemistry Research Group is to conduct world-leading research to gain an understanding of the natural processes which determine chemical evolution in the molecular clouds of deep space and on the celestial bodies of planetary systems.
We also support space missions by studying the radiation effects on materials relevant to satellite technology and future Lunar and Martian settlements, as well as the functional changes in space-borne materials that support space exploitation.
The ATOMKI Solar-Wind Simulator
Among the processes which determine the chemical evolution in the molecular clouds of deep space and on the celestial bodies of planetary systems are those induced by radiation. At ATOMKI we model ion impact processes on icy and other solar system relevant surfaces using our SOlar-Wind Simulator (SOWS).
The Sun emits a stream of charged particles known as the solar (or stellar) wind. Most of them are protons and electrons, but heavier ions also make a significant contribution to it. In the figure, the energy spectra of those heavier ions are shown, measured by NASA satellites. The proton spectrum is not shown, but it is about one order of magnitude more intense than that of helium.
SOWS is composed of simulation chambers attached to one of ATOMKI’s accelerators. ICA at the Tandetron, and AQUILA at the ECR ion source. The grey inset in the figure shows the energy ranges covered by the particle accelerators. We are currently planning to replace our old high voltage platform with a mid-energy range accelerator (MERA). It will be equipped with two astrochemistry stations, one of them at the end of a vertical beamline for irradiating, e.g., powder samples, like Lunar regolith analogues.
Experimental Facilities
ICE CHAMBER FOR ASTROPHYSICS / ASTROCHEMISTRY (ICA)
The ICA experimental setup at Atomki is designed to investigate the ion irradiation of interstellar and Solar System ice analogues, deposited on a series of cold substrates. Ions of different species and charge states are produced by the Atomki Tandetron accelerator and may be used to mimic the effect of galactic cosmic rays and stellar winds. The ice composition and the physico-chemical changes induced upon ion irradiation are monitored by infrared spectroscopy. Temperature programed desorption studies may also be performed on both non-irradiated and irradiated ices. The goal of the experimental apparatus is to systematically study space relevant ices under different ion-impact conditions to better understand the origin and evolution of the building blocks of life.
ATOMKI-QUEENS UNIVERSITY ICE CHAMBER FOR LABORATORY ASTROCHEMISTRY (AQUILA)
The AQUILA facility is established to perform ion irradiation studies of astrophysical ice analogues. It consists of a UHV-compatible chamber containing a substrate on which astrophysical ice analogues can be grown at cryogenic temperatures (≥20K). Such ices can then be processed via ion irradiation. The ECRIS Laboratory can produce all known components of the solar wind, along with highly charged ions and certain negative or molecular ions. The resultant chemical or physical changes in the ice may be monitored using mid-infrared spectroscopy. Temperature programed desorption studies may also be performed. The goal of the experimental apparatus is to systematically study space relevant ices under different ion-impact conditions.
FACILITY FOR REFRACTIVE OPTICS DENSITY AND SPUTTERING TESTS (FROST)
This set-up is designed to investigate the optical and physical properties of ices relevant to astrochemistry and molecular astrophysics. It is comprised of a UHV experimental chamber with a cryogenic sample holder, a two-laser interferometry system, and a cryogenic quartz-crystal microbalance (CQCM). The thickness and refractive index of an ice layer can be measured dynamically by the two-laser system during its condensation onto the CQCM, and the deposited mass can be determined directly by CQCM. This allows for the density of the ice structure to be calculated. These experimental data are very sparsely reported in the literature. By varying the temperature of the substrate and deposition rate, information can be gained about ice phase transitions, and possibly also ice porosity. The chamber is presently under construction and so more information on its performance and availability will be provided in the near future.
TIME OF FLIGHT FACILITY FOR EXTRATERRESTIAL LIKE EXPERIMENTS (TOFFEE)
TOFFEE is a specialized Time-of-Flight spectrometer designed to investigate ion-induced molecular fragmentation. The core configuration is based on a Wiley-McLaren time-of-flight setup, enhanced with a specialized electrostatic extractor and an einzel lens system. Projectile ions ranging from H to are generated by the tandetron accelerator at Atomki. Experiments can be conducted using a standard crossed beam arrangement. Following collision, the charged fragments are extracted from the collision region and directed through the drift tube. These fragments are detected by a custom-made MCP detector, which records the flight times and the rough positions of the incident particles. The aim of these experiments is to systematically study the irradiation-induced dissociation of space-relevant molecules and to provide molecular-level information for ice phase studies.
FIELD FREE TIME OF FLIGHT (FFTOF)
The field-free TOF technique is a specific method for avoiding distortion fields due to contact potentials, geometric and surface charging effects. It allows measuring accurately the velocity distribution of ionic fragments from ion-impacted molecules down to 0.1-eV emission energy, thus providing double-differential cross sections for collision-induced fragment emission in the sub-eV energy range. A typical example of the method’s capabilities is that with our FFTOF it was possible to measure the molecular-rotation-induced splitting of the binary ridge in the velocity map of sub-eV H+ ions ejected from H2 molecules by ion impact.
Projects and Networking
Firmly integrated into regional, European, and global networks of international space science collaboration, ATOMKI and its Space Chemistry Research Group actively contribute as a member of the Europlanet Society and serve as the driving force behind the Hungarian Space Chemistry Research Network. In alignment with the European states’ commitment to advancing space research—recognized for its scientific and technological value to the European economy—we are dedicated to establishing ATOMKI’s laboratories as a world-class research hub. This vision is pursued through close cooperation with our international partners, ensuring a leading role in this rapidly evolving field.
Recent publications
Hydroxylamine in astrophysical ices: Infrared spectra and cosmic-ray-induced radiolytic chemistry
Belén Maté; Ramón J. Peláez; Germán Molpecerez; Richárd Rácz; Duncan V. Mifsud; Juan Ortigoso; Víctor M. Rivilla; Gergő Lakatos; Béla Sulik; Péter Herczku; Sergio Ioppolo; Sándor Biri; Zoltán Juhász
Abstract
Gas-phase hydroxylamine (NH2OH) has recently been detected within dense clouds in the interstellar medium. However, it is also likely present within interstellar ices, as well as on the icy surfaces of outer Solar System bodies, where it may react to form more complex prebiotic molecules such as amino acids.
Aims. In this work, we aim to provide infrared spectra of NH2OH in astrophysical ice analogues that will help in the search for this molecule in various astrophysical environments. Furthermore, we aim to provide quantitative information on the stability of NH2OH upon exposure to ionising radiation analogous to cosmic rays, as well as on the ensuing chemistry and potential formation of complex prebiotic molecules.
Methods. Ices composed of NH2 OH, H2O, and CO were prepared by vapour deposition, and infrared spectra were acquired between 4000–500 cm−1 (2.5–20 µm) prior to and during irradiation using 15 keV protons.
Results. Our spectroscopic characterisations determine that NH2OH ices deposited at 10–20 K adopt an amorphous structure, which begins to crystallise upon warming to temperatures greater than 150 K. In interstellar ice analogues, the most prominent infrared absorption band of NH2OH is that at about 1188 cm−1, which may be a good candidate to use in searches for this species in icy space environments. Calculated effective destruction cross-sections and G-values for the NH2 OH-rich ices studied show that NH2OH is rapidly destroyed upon exposure to ionising radiation (more rapidly than a number of previously studied organic molecules) and that this destruction is slightly enhanced when it is mixed with other icy species. The irradiation of a NH2OH:H2O:CO ternary ice mixture leads to a rich chemistry that includes the formation of simple inorganic molecules such as NH3, CO2, OCN−, and H2O2, as well as ammonium salts and, possibly, complex organic molecules relevant to life such as formamide, formic acid, urea, and glycine.
An Arctic analogue for the future exploration of possible biosignatures on Enceladus
F. Franchi; M. Túri; G. Lakatos; K. K. Rahul; D.V. Mifsud; G. Panieri; R. Rácz; S.T.S. Kovács; E. Furu; R. Huszánk; R. W. McCullough; Z. Juhász
Abstract
Methane-rich emissions to the seafloor along the Arctic mid-oceanic ridge hold strong astrobiological significance, as they may represent analogues of putative hydrothermal vent environments on Enceladus. Although such environments on Enceladus would be ideal to sample in future astrobiological missions, this may not be possible due to technological and logistical limitations. As such, searching for biosignatures in the more readily sampled cryovolcanic plumes or Enceladus’ icy shell is preferable. In this regard, the Arctic Ocean, where the geologically active seafloor is covered by thousands of metres of salty water and sealed by an ice cap, is a unique terrestrial analogue of Enceladus. In the present study, we have sought to determine whether any geochemical biosignatures associated with methane cycling (e.g., elevated methane concentrations, carbon isotopic fractionation) can be detected in Arctic ice and seawater samples using mass spectrometric techniques similar to those likely to be included in the payloads of planned missions to Enceladus. Our results have shown that, although no unequivocal evidence of methane could be detected in our Arctic samples, the carbon isotopic composition of carbon dioxide gas and the oxygen isotopic composition of water vapour emitted from the Arctic samples could indeed be measured. Furthermore, an excess of molecular hydrogen with abundances comparable to the composition of Enceladus’ southern pole plume was possibly observed in one of the Arctic ice samples. These results have implications for detectable indirect geochemical evidence of putative ecosystems of hydrogenotrophic methanogenic life on the seafloor of Enceladus and justify future efforts at method development and refinement using apparatus similar to that likely to be included in the payloads of future missions.
AQUILA: A laboratory facility for the irradiation of astrochemical ice analogs by keV ions
R. Rácz; S. T. S. Kovács; G. Lakatos; K. K. Rahul; D. V. Mifsud; P. Herczku; B. Sulik; Z. Juhász; Z. Perduk; S. Ioppolo; N. J. Mason; T. A. Field; S. Biri; R. W. McCullough
Abstract
The detection of various molecular species, including complex organic molecules relevant to biochemical and geochemical processes, in astronomical settings, such as the interstellar medium or the outer solar system, has led to the increased need for a better understanding of the chemistry occurring in these cold regions of space. In this context, the chemistry of ices prepared and processed at cryogenic temperatures has proven to be of particular interest due to the fact that many interstellar molecules are believed to originate within the icy mantles adsorbed on nano- and micro-scale dust particles. The chemistry leading to the formation of such molecules may be initiated by ionizing radiation in the form of galactic cosmic rays or stellar winds, and thus, there has been an increased interest in commissioning experimental setups capable of simulating and better characterizing this solid-phase radiation astrochemistry. In this article, we describe a new facility called AQUILA (Atomki-Queen’s University Ice Laboratory for Astrochemistry), which has been purposefully designed to study the chemical evolution of ices analogous to those that may be found in the dense interstellar medium or the outer solar system as a result of their exposure to keV ion beams. The results of some ion irradiation studies of CH3OH ice at 20 K are discussed to exemplify the experimental capabilities of the AQUILA as well as to highlight its complementary nature to another laboratory astrochemistry setup at our institute.
