Asteroid fragmentation approaches for modeling atmospheric energy deposition

Register, Paul J.; Mathias, Donovan; Wheeler, Lorien

doi:10.1016/j.icarus.2016.11.020

Cited by 61 publications

(53 citation statements)

References 13 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…; Bland and Artemieva ; Ceplecha and Revelle ; Register et al. and many others). Fragmentation occurs when dynamic pressure exceeds fragment strength.…”

Section: Fragmentation Modelingmentioning

confidence: 92%

The Maribo CM2 meteorite fall—Survival of weak material at high entry speed

Borovička

Попова

Spurný

2019

Meteorit & Planetary Scien

View full text Add to dashboard Cite

High entry speed (>25 km s À1 ) and low density (<2500 kg m À3 ) are the two factors that lower the chance of a meteoroid to drop meteorites. The 26 g carbonaceous (CM2) meteorite Maribo recovered in Denmark in 2009 was delivered by a bright bolide observed by several instruments across northern and central Europe. By reanalyzing the available data, we confirmed the previously reported high entry speed of (28.3 AE 0.3) km s À1 and trajectory with slope of 31°to the horizontal. In order to understand how such a fragile material survived, we applied three different models of meteoroid atmospheric fragmentation to the detailed bolide light curve obtained by radiometers located in Czech Republic. The Maribo meteoroid was found to be quite inhomogeneous with different parts fragmenting at different dynamic pressures. While 30-40% of the (2000 AE 1000) kg entry mass was destroyed already at 0.02 MPa, another 25-40%, according to different models, survived without fragmentation up to the relatively large dynamic pressures of 3-5 MPa. These pressures are only slightly lower than the measured tensile strengths of hydrated carbonaceous chondrite (CC) meteorites and are comparable with usual atmospheric fragmentation pressures of ordinary chondritic (OC) meteoroids. While internal cracks weaken OC meteoroids in comparison with meteorites, this effect seems to be absent in CC, enabling meteorite delivery even at high speeds, though in the form of only small fragments.

show abstract

“…; Bland and Artemieva ; Ceplecha and Revelle ; Register et al. and many others). Fragmentation occurs when dynamic pressure exceeds fragment strength.…”

Section: Fragmentation Modelingmentioning

confidence: 92%

The Maribo CM2 meteorite fall—Survival of weak material at high entry speed

Borovička

Попова

Spurný

2019

Meteorit & Planetary Scien

View full text Add to dashboard Cite

show abstract

“…Additionally, the size and behavior of the flow field strongly depends on whether the shock envelope encompasses both primary and secondary fragments (e.g., Laurence et al, 2007; 3. Hybrid models (e.g., Register et al, 2017;Wheeler et al, 2017). These models combine the advantages of both discrete fragmentation and hydrodynamic approach to account for the flow field evolution and energy deposition by individual fragments, dust particles and ablated vapor and plasma.…”

Section: Meteoroid Fragmentationmentioning

confidence: 99%

Physics of meteor generated shock waves in the Earth’s atmosphere – A review

Silber

Boslough

Hocking

et al. 2018

Advances in Space Research

101

View full text Add to dashboard Cite

Shock waves and the associated phenomena generated by strongly ablating meteoroids with sizes greater than a few millimeters in the lower transitional flow regime of the Earth's atmosphere are the least explored aspect of meteor science. In this paper, we present a comprehensive review of literature covering meteor generated shock wave phenomena, from the aspect of both meteor science and hypersonic gas dynamics. The primary emphasis of this review is placed on the mechanisms and dynamics of the meteor shock waves. We discuss key aspects of both shock generation and propagation, including the great importance of the hydrodynamic shielding that develops around the meteoroid. In addition to this in-depth review, the discussion is extended to an overview of meteoroid fragmentation, followed by airburst type events associated with large, deep penetrating meteoroids. This class of objects has a significant potential to cause extensive material damage and even human casualties on the ground, and as such is of great interest to the planetary defense community. To date, no comprehensive model exists that accurately describes the flow field and shock wave formation of a strongly ablating meteoroid in the non-continuum flow regime. Thus, we briefly present the current state of numerical models that describe the comparatively slower flow of air over non-ablating bodies in the rarefied regime. In respect to the elusive nature of meteor generated shock wave detection, we also discuss relevant aspects and applications of meteor radar and infrasound studies as tools that can be utilized to study meteor shock waves and related phenomena. In particular, infrasound data can provide energy release estimates of meteoroids entering the Earth's atmosphere. We conclude with a summary of unresolved questions in the domain of meteor generated shock waves; topics which should be a focus of future investigations in the field.

show abstract

“…A graphic representation of the different fragmentation models: Instantaneous (a) Common Bowl (b), Halved (c), Pancake (d), and Single Bowl (e). More details on the fragmentation models can be found in (Register et al 2017).…”

Section: Different Fragmentation Modelsmentioning

confidence: 99%

The Deposition of Heavy Elements in Giant Protoplanetary Atmospheres: The Importance of Planetesimal–Envelope Interactions

Valletta¹,

Helled²

2019

ApJ

View full text Add to dashboard Cite

In the standard model for giant planet formation, the planetary growth begins with accretion of solids followed by a buildup of a gaseous atmosphere as more solids are accreted, and finally, by rapid accretion of gas. The interaction of the solids with the gaseous envelope determines the subsequent planetary growth and the final internal structure. In this work we simulate the interaction of planetesimals with a growing giant planet (proto-Jupiter) and investigate how different treatments of the planetesimal-envelope interaction affect the heavy-element distribution, and the inferred core mass. We consider various planetesimal sizes and compositions as well as different ablation and radiation efficiencies, and fragmentation models. We find that in most cases the core reaches a maximum mass of ∼ 2 M ⊕ . We show that the value of the core's mass mainly depends on the assumed size and composition of the solids, while the heavy-element distribution is also affected by the fate of the accreted planetesimals (ablation/fragmentation). Fragmentation, which is found to be important for planetesimals > 1 km, typically leads to enrichment of the inner part of the envelope while ablation results in enrichment of the outer atmosphere. Finally, we present a semi-analytical prescription for deriving the heavy-element distribution in giant protoplanets.

show abstract

Asteroid fragmentation approaches for modeling atmospheric energy deposition

Cited by 61 publications

References 13 publications

The Maribo CM2 meteorite fall—Survival of weak material at high entry speed

The Maribo CM2 meteorite fall—Survival of weak material at high entry speed

Physics of meteor generated shock waves in the Earth’s atmosphere – A review

The Deposition of Heavy Elements in Giant Protoplanetary Atmospheres: The Importance of Planetesimal–Envelope Interactions

Contact Info

Product

Resources

About