Precise Model for Small-Body Thermal Radiation Pressure Acting on Spacecraft

Hesar, Siamak G.; Scheeres, Daniel J.; McMahon, Jay W.; Rozitis, B.

doi:10.2514/1.g002566

Cited by 7 publications

(4 citation statements)

References 23 publications

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“…The TRP model used is from Hesar et al () but simplified for a cannonball particle instead of a complex spacecraft shape as in that work. The acceleration can be computed as

{bolda}_{t h} = - \frac{false(1 + α false) A}{m} true \sum_{i \in F}^{N_{F}} P_{i} \frac{false(boldr - {boldr}_{i} false)}{false| boldr - {boldr}_{i} false|},

where the summation goes over the number of facets of the shape model, N F , whose positions are referenced on the body by the position of their centers, r i .…”

Section: Dynamic Modelingmentioning

confidence: 99%

“…The TRP model used is from Hesar et al (2017) but simplified for a cannonball particle instead of a complex spacecraft shape as in that work. The acceleration can be computed as…”

Section: Thermal Radiation Pressurementioning

confidence: 99%

“…The fate of the ejecta is strongly controlled by the effects of SRP, which has also been found by Garcia Yarnoz et al (). While these works are relevant and provide valuable insight, it is crucial to include two other effects to get realistic results, especially for low‐altitude particles: shadowing from the primary body which turns off SRP when eclipsed (Russell et al, ), and thermal radiation pressure forces from the infrared radiation leaving Bennu (Hesar et al, ).…”

Section: Introductionmentioning

confidence: 99%

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Dynamical Evolution of Simulated Particles Ejected From Asteroid Bennu

et al. 2020

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In early 2019, the OSIRIS‐REx spacecraft discovered small particles being ejected from the surface of the near‐Earth asteroid Bennu.sww Although they were seen to be ejected at slow speeds, on the order of tens of cm/s, a number of particles were surprisingly seen to orbit for multiple revolutions and days, which requires a dynamical mechanism to quickly and substantially modify the orbit to prevent re‐impact upon their first periapse passage. This paper demonstrates that, based on simulations constrained by the conditions of the observed events, the combined effects of gravity, solar radiation pressure, and thermal radiation pressure from Bennu can produce many sustained orbits for ejected particles. Furthermore, the simulated populations exhibit two interesting phenomena that could play an important role in the geophysical evolution of bodies such as Bennu. First, small particles (<1 cm radius) are preferentially removed from the system, which could lead to a deficit of such particles on the surface. Second, re‐impacting particles preferentially land near or on the equatorial bulge of Bennu. Over time, this can lead to crater in‐filling and growth of the equatorial radius without requiring landslides.

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“…The TRP model used is from Hesar et al () but simplified for a cannonball particle instead of a complex spacecraft shape as in that work. The acceleration can be computed as

{bolda}_{t h} = - \frac{false(1 + α false) A}{m} true \sum_{i \in F}^{N_{F}} P_{i} \frac{false(boldr - {boldr}_{i} false)}{false| boldr - {boldr}_{i} false|},

where the summation goes over the number of facets of the shape model, N F , whose positions are referenced on the body by the position of their centers, r i .…”

Section: Dynamic Modelingmentioning

confidence: 99%

“…The TRP model used is from Hesar et al (2017) but simplified for a cannonball particle instead of a complex spacecraft shape as in that work. The acceleration can be computed as…”

Section: Thermal Radiation Pressurementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Dynamical Evolution of Simulated Particles Ejected From Asteroid Bennu

et al. 2020

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“…Applications of thermal radiation pressure in similar contexts are presented in McMahon et al (2020) (see Lauretta et al 2019 for the activity of Bennu) and the spacecraft control A&A 654, A113 (2021) (Hesar et al 2017). However, the formalisms in those works are applicable only to large particles (geometric regime) at large initial height (typically around 10 m).…”

Section: Introductionmentioning

confidence: 95%

Thermal radiation pressure as a possible mechanism for losing small particles on asteroids

Bach

Ishiguro

2021

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Context. Recent observations of dust ejections from active asteroids, including (3200) Phaethon, have drawn considerable interest from planetary astronomers studying the generation and removal of small dust particles on asteroids. Aims. In this work, we aim to investigate the importance of thermal radiation pressure from asteroid regolith (AR) acting on small dust particles over the surface of the AR. In particular, we aim to understand the role of thermal radiation in the near-Sun environment. Methods. We describe the acceleration of particles over the AR within the radiation fields (direct solar, reflected (scattered) solar, and thermal radiation) in addition to the asteroid’s rotation and gravitational field. Mie theory is used because the particles of interest have sizes comparable to thermal wavelengths (~1–100 μm), and thus the geometric approximation is not applicable. A new set of formalisms is developed for the purpose. Results. We find that the acceleration of particles with spherical radius ≲1 μm to ~10 μm is dominated by the thermal radiation from the AR when the asteroid is in the near-Sun environment (heliocentric distance rh ≲ 0.8 au). Under thermal radiation dominance, the net acceleration is towards space, that is, outwards from the AR. This outward acceleration is the strongest for particles of ~1 μm in radius, regardless of other parameters. A preliminary trajectory integration using the Phaethon-like model shows that such particles escape from the gravitational field within about 10 min. Our results are consistent with the previous observational studies on Phaethon in that the ejected dust particles have a spherical radius of ~1 μm.

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