Wow, what an Astronomy & Astrophysics for Nov. (vol. 703):
Ortiz, J. L. Morales, N. Sicardy, B. et al. A high geometric albedo and small size for the Haumea cluster member (24835) 1995 SM55 determined from a stellar occultation and photometric… A147 202556498
Liu, J. Wang, X. Tang, Y. et al. Volatile distribution inversion and rotation analysis of comet 103P/Hartley 2 using nongravitational effects A120 202554487
Moeslinger, A. Gunell, H. Stenberg Wieser, G. et al. Kinetic-scale physics of multi-species solar wind – Interaction with a comet A173 202452636
Marčeta, D. Novaković, B. Gavrilović, M. Numerical validation of the Yarkovsky effect in super-fast rotating asteroids A185 202556297
Le Pivert-Jolivet, T. de León, J. Licandro, J. et al. Compositional characterisation of asteroid (84) Klio with JWST A211 202555973
Jin, S. Ishiguro, M. Simulation of impact-induced seismic shaking on asteroid (25143) Itokawa to address its resurfacing process A212 202555854
Zhang, T. Tang, H. Li, X. et al. Formation of np-Fe0 particles by H+ irradiation: Insight into space weathering on the moon and other airless bodies A213 202555249
Smirnov, E. Milić Žitnik, I. High-order mean-motion resonances in the main belt A237 202557400
Sfair, R. Pinheiro, T. F. L. L. Ramon, G. et al. The resilience of the sailboat stable region A266 202555889
Wargnier, A. Simon, P. N. Fornasier, S. et al. Deimos photometric properties: Analysis of 20 years of observations (2004-2024) by the Mars Express HRSC camera A289 202555564
de Dios-Cubillas, A. Prieto-Ballesteros, O. López, I. et al. The formation of clathrites under planetary conditions of ocean worlds: The case of Ceres and implications for future missions A297 202556029
Sergeyev, A. V. Carry, B. Eggl, S. et al. Rotation periods of asteroids serendipitously observed by the NASA/Kepler K2 mission A302 202554052
Takahashi, J. Itoh, Y. Tozuka, M. et al. POPO: Fast-modulating polarimeter with imaging capability A265 202555724
Rizos, J. L. Ortiz, J. L. Gutierrez, P. J. et al. An open-access web tool for light curve simulation and analysis of small Solar System objects A178 202556525
I usually don’t get involved with TNOs, but here we are. Read Ortiz et al. and to an extent Sfair et al. if you feel. Their techniques are also applicable to within-Neptune objects.
The Giotto mission could not ‘weigh’ Halley’s Comet, via radio science- they flew past each other too fast. Instead, a mass for the Halley nucleus got derived, from observing jetting effects pushing on the unobserved mass. Liu et al. do similarly for Comet Hartley 2.
The Rosetta mission didn’t unlock comet activity… but it did study heliospherics and solar wind interactions. Moeslinger et al. hypothesize interactions with nontrivial solar winds.
Marčeta et al.: pretty cut-and-dried from the title. They compare Yarkovsky calculations to observations of actual asteroid spinning/orbiting. Result: yeah, we understand the Yarkovsky effect pretty well.
We have Ryugu samples, and we have Bennu samples… what of the other (x00,000-x,000,000) carbonaceous asteroids (including asteroid-comet transition objects)? (84) Klio is one, seen only from Earth-vicinity telescopes. But JWST is one of those ‘scopes, showing phyllosilicates and carbonates, like on Ryugu and Bennu. And possibly more…
Speaking of rubble-pile asteroids: we saw rubble sorting on Itokawa, via the Hayabusa mission. Large and small grains sorted out, we think via shaking (the Brazil-Nut Effect?). Jin et al. continue here.
Speaking of Itokawa: grains from Itokawa, returned by Hayabusa, were a clear demonstration of space weathering: surfaces of exposed grains showed nanophase iron, ‘smelted’ from iron ‘ore’ by the action of the solar wind and micrometeorites. Zhang et al. continue here.
Speaking of asteroid orbital dynamics: other eastern Europeans, like Marčeta et al., consider higher-order effects than simple Keplerian orbits… higher-higher order. A surprising amount of the Main Belt is in (weak) resonance with something.
Deimos is not an asteroid, because it’s a natural satellite of Mars… or is it? Did Mars capture Deimos as it was passing? Either way, Deimos and Phobos have been used as stand-ins for asteroids since the ’70s, before we could visit ‘real’ asteroids. Since we happen to have instruments at Mars, we (at least, Wargnier et al.) turn them towards Phobos and, to a lesser extent, Deimos.
Ceres: the nearest ocean world (we think…). Strange chemistries may be possible in exo-oceans, or not-so-strange: de Dios-Cubillas et al. consider clathrites, already seen on Earth in some seabed deposits.
Telescopes: good for multiple things. In the Kepler mission’s case, pointing a ‘scope at a big patch of space just happens to catch some asteroids (as it should). Sergeyev et al. report what they caught.
Speaking of telescopes, Takahashi et al. have a new instrument. This just happens to be useful at asteroids, where polarimetry can be used to derive multiple properties.
Even more basic than telescopes are algorithms and code. Rizos et al. report their code for light curves, used to measure the spin of (nonspherical) asteroids and comet nuclei as they brighten and darken. To higher degrees, good-quality data may reveal spin axes, binarity, etc.
Whew!