ASPACE-Q 

The Astrophysics,  Space  Exploration and Quantum Computing Group   

 ASPACE-Q 

The Astrophysics,  Space  Exploration and Quantum Computing Group   

by Monica Scorța, ing

03.11.2025

Product Assurance (PA) and Quality Assurance (QA) are processes that aim to ensure compliance with specific applicable requirements and quality standards throughout the lifecycle of a space mission. The requirements can be perceived as the necessities that the persons in charge of the mission commit to fulfil for reaching its success. Key activities in the PA/QA processes include the establishment of clear quality goals (clear milestones to target), creation of processes and procedures to be followed by each team involved in a space mission, and implementation of preventive activities for continuous monitoring and assessment of the mission’s integrity and favourable outcome 

Like other standards used across industries (ISO manufacturing, healthcare, information technology, and ANSI - telecommunications, energy, finance), the ones used for the LISA Mission are the widely accepted ones used in the European space-missions framework, the ECSS (The European Cooperation for Space Standardization) standards. They approach thematics like Space Management, Space Engineering, and Space Sustainability, helping the involved teams in guiding themselves in the evolution process of the mission, from the very beginning, where the scene is set, the Conceptual Study, to the very end, the Disposal/Debris Mitigation.


The ECSS documentation is formed by a series of Standards, Handbooks, and Technical Memoranda that address, in turn, requirements to be applied for each existing context of a space mission, additional information for the application of different standards, and non-normative but useful technical aspects to take into account. From these upper-level documents, there can be obtained the refined of, with the associated requirements, namely the so-called Tailored Requirements. These tailored requirements are a subset of the generic standards found in the ECSS documentation, aiming at addressing specific needs of the mission, in specific contexts, and reaching particular goals of the project.

LISA has its own Tailored Requirements that are followed by all the parties involved in the process of this mission’s realization. This user-friendly, single set of standards applied through the PA/QA activities is part of the LISA’s Product Assurance and Quality Assurance team’s activities, of whose members work in the ASPACE-Q group. There are these collective work and split responsibilities across the collaboration to ensure compliance with the ECSS standards and the Tailored Standards for the fulfilment of the mission.

Given the complexity of this endeavour, a planned approach to the necessary tasks to be fulfilled has always been the way to go in the context of space missions and not only. 








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by Alice Păun, PhD student

19.09.2025














Image courtesy of: Bureau of International Cooperation, Chinese Academy of Sciences


Although binary systems consisting of a pulsar and a helium star have been observed before, never until now has such a binary system been observed right in our own galaxy. In 2021, the FAST (Five-hundred-meter Aperture Spherical radio Telescope), during the “Galactic Plane Pulsar Snapshot survey”, observed an eclipse of the pulsar PSR J1928+1815.
At present, there is not yet a complete understanding of how these binary systems form and evolve. According to what we know, however, in a binary system of two stars, one of them tends to expand so that its atmosphere envelopes the other. As mass is transferred from one star to the other, their orbit shrinks over a period of approximately 1000 years, and the next stage is either that the two stars merge or, alternatively, that this atmosphere is ejected.

Considering the case observed with FAST, the binary system is composed of a star – neutron-star pair, and in these conditions, when the atmosphere is ejected, a helium star and a pulsar are formed. The latter is a neutron star that rotates rapidly and emits pulses in the radio band at a rate of hundreds of pulses per second. Thus, the helium star can eclipse the pulsar over the course of its orbit around it, causing “gaps” in its detection due to the shielding of the emitted radio signal. The time it takes for the two stars to complete one orbit around each other is 3.6 hours, and for 1/6 of this period, the pulsar is eclipsed and its signal cannot be detected.

















Image source: Z. L. Yang et al. Science388,859-863(2025). DOI:10.1126/science.ado0769


Over time, this binary system evolves into a system made up of two compact objects that merge and generate a new source of gravitational waves.


















Image source: Z. L. Yang et al. Science388,859-863(2025). DOI:10.1126/science.ado0769


References:

1.    Z. L. Yang et al., A pulsar-helium star compact binary system formed by common envelope evolution. Science388,859-863(2025). DOI:10.1126/science.ado0769

2.    https://physicsworld.com/a/short-lived-eclipsing-binary-pulsar-spotted-in-milky-way/

by Maria Ișfan, PhD student

12.09.2025

Top Left: 3D atomistic model of the graphene device. Bottom Left: Top view of the actual device, as seen under an optical microscope. Right: Artistic Illustration of electrons moving like a fluid inside graphene. Credit: Aniket Majumdar

Researchers at the Department of Physics, Indian Institute of Science (IISc), and collaborators from the National Institute for Material Science in Japan detected for the first time a quantum fluid of electrons in graphene (a material structure made of a single layer of carbon atoms). The results were published in Nature Physics (https://www.nature.com/articles/s41567-025-02972-z).


These electrons behave like a Dirac fluid. Instead of acting like individual quantum particles, they flow collectively as an ultra-low viscosity fluid. Usually, in a material the electrical and the thermal conductivities are proportional. However, in this electron fluid, they have an inverse relation, violating the Wiedermann-Franz law with a factor larger than 200 at low temperatures.


This exotic state of matter resembles the quark-gluon plasma, which is observed in particle accelerators at CERN.

by Florentina Pîslan, PhD student

03.11.2025

On the night of September 7–8, 2025, the longest total lunar eclipse in recent decades took place. More precisely, the phenomenon lasted 82 minutes and could be observed by about 85% of the world’s population, including from Romania!

Credit imagine: Maximilian Teodorescu, cercetător la Institutul de Științe Spațiale - filiala INFLPR

A total lunar eclipse occurs when, during its orbit around Earth, the Moon passes behind the planet, causing Earth to completely shadow it. The only light that still reaches the Moon is that which first passes through Earth’s atmosphere, which filters the wavelengths of sunlight. As a result, only the longer wavelengths, such as red and orange, reach the Moon’s surface, while the shorter wavelengths, such as blue and violet, scatter more easily and do not reach it. Consequently, during a total eclipse, the Moon appears reddish, which is why it is often called a ‘Blood Moon.’




Sursă imagine: NASA Goddard Space Flight Center/Scientific Visualization Studio

29.08.2025

by Florin-Ioan Constantin, Ph.D. student


source: https://www.esa.int/Space_Safety/Planetary_Defence/Ramses_ESA_s_mission_to_asteroid_Apophis






This week, the European Space Agency (ESA) announced the intention of the Japanese Space Agency (JAXA) to collaborate with ESA on the RAMSES mission (Rapid Apophis Mission for Space Safety).

The asteroid Apophis has a diameter of approximately 375 meters and was discovered in 2004. On April 13, 2029, it will pass close to our planet at a distance of about 32,000 kilometers, allowing us to see it with the naked eye for a short time from Europe, Africa, and parts of Asia during its passage.

The RAMSES mission aims to intercept asteroid Apophis during its 2029 flyby of Earth in order to study its properties as it comes under the influence of our planet’s gravitational pull. The proposal for this mission is scheduled to be reviewed by ESA in November 2025, and if approved, it will launch in 2028 to rendezvous with the asteroid before it enters Earth’s gravitational field. Scientists expect our planet’s gravity to alter the way the asteroid spins as it travels, which could in turn trigger quakes and landslides on its surface. Thus, RAMSES will provide critical information about the asteroid’s condition before these additional gravitational influences, about their direct effects, and about the final outcome and long-term consequences that may result.

This mission also builds on and refines part of the technology and scientific developments that led to the adoption and launch of another similar mission, HERA, which was launched in 2024 and is currently en route to the asteroid Dimorphos, part of the Didymos binary asteroid system.



Sources and further reading:

https://www.esa.int/Space_Safety/Planetary_Defence/ESA_and_JAXA_advance_potential_Apophis_mission_collaboration

https://www.esa.int/Space_Safety/Planetary_Defence/Ramses_ESA_s_mission_to_asteroid_Apophis

https://www.reuters.com/business/aerospace-defense/japan-provide-h3-rocket-europes-mission-observe-apophis-asteroid-2025-08-22/



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