scholarly journals Cavezzo, the first Italian meteorite recovered by the PRISMA fireball network. Orbit, trajectory, and strewn-field

2020 ◽  
Vol 501 (1) ◽  
pp. 1215-1227 ◽  
Author(s):  
D Gardiol ◽  
D Barghini ◽  
A Buzzoni ◽  
A Carbognani ◽  
M Di Carlo ◽  
...  
Keyword(s):  
Observational Data ◽  
Total Mass ◽  
Bright Light ◽  
Network Data ◽  
Orbital Elements ◽  
Two Samples ◽  
Original Mass ◽  
Near Earth Asteroids ◽  
The Town ◽  
Light Flashes

ABSTRACT Two meteorite pieces have been recovered in Italy, near the town of Cavezzo (Modena), on 2020 January 4th. The associated fireball was observed on the evening of New Year’s Day 2020 by eight all-sky cameras of the PRISMA fireball network, a partner of FRIPON. The computed trajectory had an inclination angle of approximately 68° and a velocity at infinity of 12.8 km s−1. Together with the relatively low terminal height, estimated as 21.5 km, those values were indicating the significant possibility of a meteorite dropping event, as additionally confirmed by the non-zero residual total mass. The strewn-field was computed taking into account the presence of two bright light flashes, revealing that the meteoroid had been very likely subject to fragmentation. Three days after the event, two samples, weighing 3.1 and 52.2 g, were collected as a result of a dedicated field search and thanks to the involvement of the local people. The two pieces were immediately recognized as freshly fallen fragments of meteorite. The computed orbital elements, compared with the ones of known Near-Earth Asteroids from the NEODyS database, are compatible with one asteroid only; 2013 VC10. The estimated original mass of the meteoroid, 3.5 kg, and size, approximately 13 cm, is so far the smallest among the current 35 cases in which meteorites were recovered from precise strewn-field computation thanks to observational data. This result demonstrates the effectiveness of accurate processing of fireball network data even on challenging events generated by small size meteoroids.

Statistical results on discovered near-Earth asteroids

1999 ◽  
Vol 173 ◽  
pp. 81-86
Author(s):  
S. Berinde
Keyword(s):  
Dynamical Evolution ◽  
Minor Planet ◽  
Orbital Elements ◽  
The Earth ◽  
Near Earth Asteroids ◽  
Statistical Results

AbstractThe first part of this paper gives a recent overview (until July 1st, 1998) of the Near-Earth Asteroids (NEAs) database stored at Minor Planet Center. Some statistical interpretations point out strong observational biases in the population of discovered NEAs, due to the preferential discoveries, depending on the objects’ distances and sizes. It is known that many newly discovered NEAs have no accurately determinated orbits because of the lack of observations. Consequently, it is hard to speak about future encounters and collisions with the Earth in terms of mutual distances between bodies. Because the dynamical evolution of asteroids’ orbits is less sensitive to the improvement of their orbital elements, we introduced a new subclass of NEAs named Earth-encounter asteroids in order to describe more reliably the potentially dangerous bodies as impactors with the Earth. So, we pay attention at those asteroids having an encounter between their orbits and that of the Earth within 100 years, trying to classify these encounters.

scholarly journals Observational Data and Orbits of the Asteroids Discovered at the Molėtai Observatory in 2008–2009

2016 ◽  
Vol 25 (4) ◽  
Author(s):  
K. Černis ◽  
I. Wlodarczyk ◽  
J. Zdanavičius
Keyword(s):  
Observational Data ◽  
Minor Planet ◽  
Orbital Elements ◽  
Main Belt ◽  
Ccd Observations ◽  
Near Earth Objects ◽  
Asteroids And Comets

AbstractWe present the statistics of the asteroids observed and discovered at the Molėtai Observatory, Lithuania, in 2008–2009 within the project for astrometric observations of the near-Earth objects (NEOs), the main belt asteroids and comets. CCD observations of the asteroids were obtained with the 35/51-cm Maksutov-type meniscus telescope. In the Minor Planet Circulars and the Minor Planet Electronic Circulars (2008–2009), 11 900 astrometric positions of 2522 asteroids were published. Among them 95 were new asteroids, including four belonging to the Trojan group: (352655) 2008QX28, 2008 SE8, (353194) 2009 SM100 and (264068) 2009 SQ148. For the asteroids discovered at Molėtai their precise orbits are calculated. Because of short observational arc, a few asteroids have low-precision orbits and some asteroids are considered lost. For the three Main Belt asteroids with low-precision orbital elements, 2008 QP32, 2008 SD8 and 2008 SG150, we present their ephemerides for 2017. They can be brighter than 20 mag.

Observational Data and Orbits of the Asteroids Discovered at the Baldone Observatory in 2008–2013

2015 ◽  
Vol 24 (3) ◽  
Author(s):  
K. Černis ◽  
I. Wlodarczyk ◽  
I. Eglitis
Keyword(s):  
Observational Data ◽  
Ccd Camera ◽  
Minor Planet ◽  
Orbital Elements ◽  
Main Belt ◽  
Schmidt Telescope ◽  
Ccd Observations ◽  
Near Earth Objects ◽  
Asteroids And Comets

AbstractThe paper presents statistics of the asteroids observed and discovered at the Baldone Observatory, Latvia, in 2008–2013 within the project for astrometric observations of the near-Earth objects (NEOs), the main belt asteroids and comets. CCD observations of the asteroids were obtained with the 0.80/1.20 m, f/3 Schmidt telescope and a ST-10XME 15 × 10 mm CCD camera. In the Minor Planet Circulars and the Minor Planet Electronic Circulars (2008–2013) we published 3511 astrometric positions of 826 asteroids. Among them, 43 asteroids were newly discovered at Baldone. For 36 of these asteroids the precise orbits are calculated. Because of short observational arc and small number of observations, a few asteroids have low-precision orbits and their tracks have been lost. For seven objects with poorly known orbits we present their ephemerides for 2015–2016. The orbits and the evolution of orbital elements of two asteroids, (428694) 2008 OS9 from the Apollo group and the Centaur (330836) Orius (2009 HW77), are recalculated including new observations obtained after 2011.

scholarly journals Spectrum Analysis of the Binary Star 53 Aur with a CP3 Component

1993 ◽  
Vol 138 ◽  
pp. 161-164
Author(s):  
Juraj Zverko ◽  
Ján Budaj ◽  
Milan Zboril ◽  
Jozef Žižňovský
Keyword(s):  
Spectrum Analysis ◽  
Total Mass ◽  
Binary Star ◽  
Rotational Velocity ◽  
High Dispersion ◽  
Orbital Elements ◽  
Binary Nature ◽  
Different Types ◽  
Magnitude Difference

The CP-star 53 Aur (HD 47152, HR 2425) has been assigned in the literature different types of peculiarity. Bertaud (1959) classified it as A0p-EuCr, Cowley et al. (1969) as B9p-Eu(Cr?), Osawa (1965) as Hg and Zverko (1974) as Mn -type. MacAlister (1978) discovered its binary nature and Tokovinin (1986) first determined its orbit with a period of 13.7 y. Subsequent interferometric observations by Baize (1989) yielded new orbital elements with a period of 25.816 y, total mass of 5.8 M⊙ and magnitude difference of two B9 components 0.3 mag. Adelman (1982) performed spectrophotometry and fitted the Balmer jump with Teff=10 500 K, while the Paschen continuum with Teff=9 500 K, log g=4 in both cases. Palmer (1965) estimated the projected rotational velocity to 325 km s−1 from the width of the Ca II-K line, while Wolff and Preston (1975) obtained 33 km s−1 from the Mg II 448.1 nm line. In this work we analyze high-dispersion spectra obtained in two distant orbital phases, namely in 1975 and in 1992 to distinguish the components of the system.

scholarly journals Mass Loss in Algol-Type Stars: Implication on their Evolutionary Stage

1982 ◽  
Vol 69 ◽  
pp. 187-189
Author(s):  
F. Mardirossian ◽  
G. Giuricin
Keyword(s):  
Mass Transfer ◽  
Angular Momentum ◽  
Mass Loss ◽  
Observational Data ◽  
Mass Exchange ◽  
Total Mass ◽  
Evolutionary Stage ◽  
Momentum Loss ◽  
Evolutionary Scenario ◽  
Angular Momentum Loss

AbstractWe have examined the observational data of 102 Algols in order to clarify the implications on their evolutionary scenario of various assumptions concerning mass and angular momentum loss during mass transfer. We have found that case B mass exchange is strongly favoured for Algols of relatively low total mass (~ M < 7 Mʘ), while case A predominates, though not so widely as expected in Algols of higher total mass.

Collisional evolution of asteroids

1999 ◽  
Vol 173 ◽  
pp. 129-144 ◽  
Author(s):  
P. Farinella ◽  
D.R. Davis ◽  
F. Marzari ◽  
D. Vokrouhlický
Keyword(s):  
High Velocity ◽  
Total Mass ◽  
Complex Mixture ◽  
Research Field ◽  
Near Earth Space ◽  
Accretion Process ◽  
High Velocity Impacts ◽  
Near Earth Asteroids ◽  
Asteroid Families ◽  
Collisional Evolution

AbstractWe review the evidence for, and the modelling work devoted to, the substantial collisional evolution which has generated the current asteroid population and continually injects asteroid fragments into dynamicalroutesthrough which they can reach near-Earth space and sometimes hit our planet. The main obstacles to further progress in this research field are theoretical (mainly related to the physics of high-velocity impacts), but better observational data (in particular on the small-size end of the asteroid population) would help. However, in the last decade new insights have been obtained on specific important issues, such as the total mass of the asteroids at the time when the accretion process was stopped (only moderately larger than the current one), the “demography” of asteroid families (how many/how old they are and how they evolve) and the way meteorites and near-Earth asteroids are delivered/transported by a complex mixture of collisional and dynamical mechanisms.

The orbital evolution of some near-Earth asteroids

1999 ◽  
Vol 173 ◽  
pp. 121-126
Author(s):  
E.I. Timoshkova
Keyword(s):  
Differential Equations ◽  
Numerical Integration ◽  
Orbital Evolution ◽  
Time Interval ◽  
Orbital Elements ◽  
Integration Procedure ◽  
Near Earth Asteroids

AbstractThe orbital evolution of the selected Near-Earth asteroids is studied by the numerical integration of the differential equations taking into account the perturbations due to all major planets for a time interval representing approximately 2000 revolutions of Jupiter. The new accurate DINCH integration procedure was used. Together with the orbital elements the Tisserand invariant is selected as a parameter to be investigated.

Astrometric observations of Near Earth Objects and Minor Planet Center

2020 ◽  
Author(s):  
Nick Sioulas
Keyword(s):  
Solar System ◽  
Proper Motion ◽  
Space Mission ◽  
Great Accuracy ◽  
Minor Planet ◽  
Orbital Elements ◽  
Dwarf Planets ◽  
A Minor ◽  
The Town ◽  
Near Earth Objects

&lt;p&gt;NOAK Observatory, Stavraki (IAU code L02) Ioannina, Greece ([email protected])&lt;/p&gt; &lt;p&gt;&lt;strong&gt;Introduction&lt;/strong&gt;&lt;/p&gt; &lt;p&gt;In this work, the astrometric observations of four asteroids will be presented which took place on 2019 from NOAK observatory located at Stavraki in Greece. The results and the procedure of submitting the measurements to MinorPlanetCenter will be discussed.&lt;/p&gt; &lt;p&gt;&lt;strong&gt;Abstract&lt;/strong&gt;&lt;/p&gt; &lt;p&gt;Astrometry is the measurement of positions, parallaxes and proper motion of an astronomical body. Especially the astrometry of Near Earth Objects (NEO) demands great accuracy and the cooperation between the professional and amateur astronomers for better results. All these objects that need confirmation are listed in the Near Earth Object Confirmation Page (NEOCP) and in the Possible Comet Confirmation Page (PCCP) at the site of the Minor Planet Center (MPC). When an object is confirmed, then a Minor Planet Electronic Circular (MPES) is published, including observations, the observers details and the orbital elements of the object. Due to the high number of the objects that need confirmation is important to use all available telescopes to track them.&lt;/p&gt; &lt;p&gt;My amateur observatory participates in the effort to record all these objects in the Solar System. The Observatory also conducts observations of various objects and other phenomena such as exoplanet transits contributing to the Ariel Space Mission with the Exoclock Project. However, the main goal of the observatory is to conduct asteroid and comet photometry and the methods, observations and results will be discussed in this presentation.&lt;/p&gt; &lt;p&gt;The observatory is registered in IAU as L02, &amp;#171;NOAK Observatory, Stavraki&amp;#187;, in the town of Ioannina, Greece.&lt;/p&gt; &lt;p&gt;&lt;strong&gt;Acknowledgements&lt;/strong&gt;&lt;/p&gt; &lt;p&gt;I would like to thank Anastasia Kokori and Angelos Tsiaras for encouraging me to publish my work and for their advice.&amp;#160;&lt;/p&gt; &lt;p&gt;&lt;strong&gt;References &lt;/strong&gt;&lt;/p&gt; &lt;p&gt;[1] Minor Planet Center: https://www.minorplanetcenter.net/&lt;/p&gt; &lt;p&gt;[2] Astrometrica: http://www.astrometrica.at/&lt;/p&gt; &lt;p&gt;[3] Roger Dymock: Asteroids and Dwarf Planets&lt;/p&gt; &lt;p&gt;[4] Brian D. Warner: A Practical Guide to Lightcurve Photometry and Analysis&lt;/p&gt; &lt;p&gt;[5] Project Pluto: https://www.projectpluto.com/&lt;/p&gt; &lt;p&gt;[6] NEODyS-2: https://newton.spacedys.com/&lt;/p&gt; &lt;p&gt;[7] Center for Near Earth Objects Studies: https://cneos.jpl.nasa.gov/&lt;/p&gt;

scholarly journals Non conservative evolutionary scenario for 100 Algols

1981 ◽  
Vol 59 ◽  
pp. 473-475
Author(s):  
F. Mardirossian ◽  
G. Giuricin
Keyword(s):  
Mass Transfer ◽  
Angular Momentum ◽  
Observational Data ◽  
Mass Exchange ◽  
Strong Evidence ◽  
Total Mass ◽  
Momentum Loss ◽  
Evolutionary Scenario ◽  
Angular Momentum Loss ◽  
Low Mass

AbstractWe have examined the observational data of 100 Algols in order to check the validity of several simple models of non-conservative mass transfer. Strong evidence of mass and angular momentum loss has been found at least in about 20% of our Algols. Case B mass exchange is favoured for low-mass Algols, while case A predominates, though not so widely as expected, in Algols of higher total mass.

scholarly journals Solving for the Orbital Elements of Binary Systems using MCMC Simulations.

2013 ◽  
Vol 8 (S299) ◽  
pp. 52-53
Author(s):  
Kyle Mede ◽  
Timothy D. Brandt
Keyword(s):  
Monte Carlo ◽  
Markov Chain ◽  
Markov Chain Monte Carlo ◽  
Observational Data ◽  
Confidence Intervals ◽  
Formation Mechanism ◽  
Binary Systems ◽  
Three Dimensional ◽  
Orbital Elements ◽  
Orbital Parameters

AbstractRecent simulation and observational data have been used to investigate the ability of Kozai oscillations to explain the formation of “hot Jupiter” planetary systems. One of the first exoplanets discovered, τ Boo Ab, orbits a star with a binary companion, making it an excellent testbed for this scenario. We have written a three-dimensional Markov Chain Monte Carlo (MCMC) simulator to constrain the orbit of the distant stellar companion τ Boo B, and are currently deriving orbital parameters and confidence intervals. These orbital parameters will confirm or reject Kozai oscillations as a plausible formation mechanism for τ Boo Ab.

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