Determination of parameters of meteor bodies based on flight observational data

Gritsevich, Maria

doi:10.1016/j.asr.2009.03.030

Cited by 70 publications

(65 citation statements)

References 10 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This conclusion is in good agreement with existing dynamic mass determination methods (e.g. Wetherill and ReVelle, 1981;Halliday et al, 1996;Gritsevich, 2009) and corresponds to the type I according to the fireball classification and PE-criterion introduced by Ceplecha and McCrosky (1976). Therefore, following the assumption made by Halliday et al (1996), for the fireballs considered in this study we accept the bulk density value of 3.5 g/cm 3 to be preferred.…”

Section: Application To the Real Phenomenasupporting

confidence: 85%

“…Therefore these two parameters can be easily determined firstly from the altitude and the body's deceleration in the atmosphere. The problem is solved using the least square method (see Gritsevich (2008aGritsevich ( , 2009 for exact formulas and details). The main advantage here is that during this part of the proposed model we do not involve any other assumptions or empirical constants.…”

Section: Altitude-velocity Relationmentioning

confidence: 99%

See 1 more Smart Citation

Constraining the luminous efficiency of meteors

Gritsevich

Koschny

2011

Icarus

View full text Add to dashboard Cite

a b s t r a c tWe propose a new approach for studying the radiation of a fireball, one of the main processes which occur when the meteor body enters the planetary atmosphere. The only quantities which directly follow from the available observations are the fireball brightness, its height above sea level, the length along the trajectory, and as a consequence its velocity as a function of time. Other important parameters like meteoroid's mass, its shape, bulk and grain density, temperature remain unknown. The present study takes recent results in fireball aerodynamics and considers them together with the classical postulate that a fraction of the meteoroid kinetic energy is transformed into radiation during its flight. This gives us a new analytical dependence, which in particular shows that the fireball luminosity in general is proportional to the body pre-entry mass value, its initial velocity to the power of 3, and the sine of the slope between horizon and trajectory. Research helps in finding an answer to the general important question: Which fraction of the fireball kinetic energy is transformed into light during meteoroid drag and ablation in the atmosphere? Ó

show abstract

Section: Application To the Real Phenomenasupporting

confidence: 85%

Section: Altitude-velocity Relationmentioning

confidence: 99%

Constraining the luminous efficiency of meteors

Gritsevich

Koschny

2011

Icarus

View full text Add to dashboard Cite

show abstract

“…). The pre‐entry mass of the Annama meteoroid was estimated based on the deceleration analysis as described by Gritsevich (, ) to be in the range of 400–500 kg (Trigo‐Rodríguez et al. ; Lyytinen and Gritsevich ), with corresponding radius around 30–35 cm.…”

Section: Introductionmentioning

confidence: 99%

Annama H chondrite—Mineralogy, physical properties, cosmic ray exposure, and parent body history

Kohout

Haloda

Halodová

et al. 2017

Meteorit & Planetary Scien

View full text Add to dashboard Cite

The fall of the Annama meteorite occurred early morning (local time) on April 19, 2014 on the Kola Peninsula (Russia). Based on mineralogy and physical properties, Annama is a typical H chondri te. It has a high Ar-Ar age of 4.4 Ga. Its cosmic ray exposure history is atypical as it is not part of the large group of H chondrites with a prominent 7 -8 Ma peak in the exposure age histograms. Instead, its exposure age is within uncertainty of a smal ler peak at 30 ±4 Ma. The results from short-lived radionuclides are compatible with an atmosperic pre-entry radius of 30 -40 cm. However, based on noble gas and cosmogenic radionuclide data, Annama must have been part of a larger body (radius >65 cm) for a large part of its cosmic ray exposure history. The 10 Be concentration indicates a recent (3 -5 Ma) breakup which may be responsible for the Annama parent body size reduction to 30 -35 cm pre-entry radius.

show abstract

“…However, as it requires detailed analysis of each meteor (including light curves and photography) it is not appropriate here. Another method, more easily automated, was recently proposed (Gritsevich, 2009;Gritsevich and Koschny, 2011). This method is entirely based on the interpretation of variations of speed and height as consequences of braking and mass loss (ablation/erosion).…”

Section: Mass From Trajectory Analysismentioning

confidence: 99%

“…While α, β and estimation of masses had already been obtained (Gritsevich, 2009) for the set of Canadian Network meteors analyzed in Section 3.4, the implementation into SAT allows us to perform the calculations with different assumptions (for mass estimation) and combine them with the latest development of the method: the determination of τ as in Gritsevich and Koschny (2011). The determination of mass and luminous efficiency requires assumption on the density ρ m .…”

Section: Script For Analysis Of Meteors Trajectories -Satmentioning

confidence: 99%