On the developmente of new viedeo stations to monitor meteorite-droppimg events over Spain

The SPanish Meteor and Fireball Network (SPMN) is an interdisciplinary project involving several universi- ties and research centres with the aim to study meteor and fireball events occurring over Spain and the bordering countries [1]. Large fireballs can be the precursors of meteorite falls and, so, the establishment of a network of detection systems is very con- venient in order to increase the chance of meteorite recovery by tracking their atmospheric trajectories and predicting the corre- sponding landing sites. To do this it is necessary to record the luminous trail from at least two different locations

Low-velocity cometary meteoroid streams encountering the earth: clues on the fragmentation of cometary aggregates and implications for interplanetary dust particles

Since 2005, the SPanish Fireball and Meteor Network (SPMN) is continuously monitor- ing meteor activity by using all-sky CCD and medium- field video cameras up to +3 to +4 meteor limiting magnitude [1,2]. One important goal of our network is the study of the meteoroid physico-chemical properties from multiple station data, together with meteor spec- tra. It is well known that the ablation behavior of me- teors in the Earth’s atmosphere shows photometric patterns that are reflecting important properties of the incoming meteoroids [3], but we are not yet fully un- derstanding such patterns. Besides, we are also trying to identify the main sources of large bolides to the Earth. As a consequence of the SPMN monitoring ef- fort, valuable trajectory and orbital data of meteors and fireballs is being obtained [4-6]. During 2007 several poorly-known meteoroid streams associated with com- ets were crossed by the Earth. We describe here unex- pected fireball activity, but focusing in low-velocity cometary streams. Particularly, we describe some me- teor outbursts and fireball events recorded by the SPMN during 2006-2007 that would be important de- livery sources of Interplanetary Dust Particles (IDPs). We try to encourage setting up future IDP campaigns for collecting cometary particles in the upper atmos- phere. By knowing the most important and favourable sources of cometary particles, and the dates of the en- counters with dense dust trails, such missions would be prepared in time for being successful

Robotic systems for meteor observing and lunar impact flashes detection in Spain

Since November 2008, a new robotic observatory is being setup by the University of Huelva within the environment of the Doñana Natural Park, in the south- west of Spain. Most of the systems in this astronomical observatory operate within the framework of the Spanish Meteor Network (SPMN), which is an interdisciplinary project dedicated to study meteoroids streams and the interaction of these particles of interplanetary matter with the Earth's atmosphere. For this we employ a system consisting of an array of high-sensitivity CCD video cameras for automatic meteor detection. Besides, an automated system for lunar impact flashes detection is being setup in collaboration with IAA-CSIC. This is based on three robotic telescopes that monitor the impact of meteoroids on the surface of the Moon. An important synergy is expected from the results recorded by both systems. Besides, climate conditions in this area provide us about 320 useful nights per year for astronomical observation, which makes this location ideal for this research project

The Northern χ -Orionid meteoroid stream and possible association with the potentially hazardous asteroid 2008XM1

We present new orbital data and dynamic results pointing towards the origin of the Northern χ -Orionid meteoroid stream, which is a part of the Taurid meteoroid complex. A new software package was developed to establish the potential parent bodies of meteoroid streams based on the similarity of their orbits. The analysis of a Northern χ -Orionid fireball observed on 2011 December 6 identified two potential parent bodies: the near-Earth object (NEO) 2002XM35 (previously proposed as the parent of this meteoroid stream) and the more recently discovered potentially hazardous asteroid 2008XM1. The calculation of the evolution of the orbital elements performed by using the Mercury 6 symplectic integrator supports the idea that 2008XM1 is a better parent body. Our data sample was expanded by including also in the calculations the mean orbit of the χ -Orionid stream. The results are consistent with the fragmentation of a larger body in the past that could give rise to both NEOs and the Northern χ -Orionid stream. To confirm this, further observations to improve the orbital elements of these asteroids should be attempted before the objects are lost. The analysis of the emission spectrum recorded for this fireball supports a primitive nature for these meteoroids.Ministerio de Ciencia e Innovación AYA2009-13227, AYA2009-14000-C03- 01, AYA2011-26522CSIC 201050I043Junta de Andalucía P09-FQM-455

A meteoroid from a Jupiter family comet recorded as a bright bolide in 2012

The continuous monitoring of meteor and fireball provides information about the origin and nature of meteoroids ablating in the Earth's atmosphere, but also about the mechanisms that deliver these materials to our planet. Thus, for instance, from the analysis of meteor events simultaneously imaged from, at least, two different locations it is possible to obtain atmospheric trajectories, radiant, orbital and physicochemical parameters such as the mass of the meteoroids and the tensile strengths of these particles [1, 2, 3]. In addition, meteor spectroscopy provides helpful information about the chemical nature of meteoroids [5, 6, 7]. With this aim, the SPanish Meteor Network (SPMN) is performing a continuous fireball monitoring and meteor spectroscopy campaign over Spain and neighbouring areas. Here we present orbital and chemical information derived from the analysis of a fireball imaged in 2012. This event was produced by a meteoroid from a Jupiter Family Comet

Spectra of bolides produced by meteoroids from (3200) phaeton

The Geminids is the densest annual meteoroid stream whose parent body is asteroid (3200) Phaethon, which was considered by some researchers as an extinct cometary nucleus rather than a regular asteroid [1]. On the basis of spectral and dynamical similarities, it has been recently proposed that asteroid 2 Pallas is the likely parent body of asteroid (3200) Phaeton [2, 3]. The asteroidal origin of the Geminids suggests that this stream could be a potential meteorite producer. The analysis of several Geminid fireballs observed between 2009 and 2010 from Spain supports this idea [4]. In this work we present the preliminary analysis of four emission spectra produced by meteoroids from the Geminids stream. These were obtained in the framework of the continuous spectroscopic campaign developed by the SPanish Meteor Network (SPMN)

A 2012 taurid bolide imaged in the framework of the Spanish fireball network

In 2010 the Spanish Meteor Net- work (SPMN) started a special program to obtain very precise orbital information on 2P/Encke meteoroids that is currently the focus of the author master thesis [1, 2]. The orbital similitude is a clear evidence on the connection between comets and meteor streams. The continuous sublimation of the ice-rich regions in cometary nuclei produces outgassing capable to re- lease cm to m-sized particles from cometary nuclei. This is the main way to produce meteoroid streams showers [3,4,5]. Another feasible physical process to produce cometary debris in heliocentric orbit is the disruption of a comet that explains the formation of about ten meteoroid streams [6,7,8]. This second pathway produces far larger particles that sometimes can even be in the meter scale and can explain very bright bolides associated with some meteor showers [8]. Unfortunately, large bolides are rare events so in order to study them a continuous sky monitoring is required which is the only way to collect information on the dynamic origin and physical behavior of large bolides penetrating Earth’s at mosphere. So far we have described different cases related to the Taurid complex [1,2]. Several Near Earth Objects (NEOs) have been dynamically associated w ith the Taurid complex clearly suggesting that the progressive disruption of a larger cometary progenitor is the source of this com- plex of bodies [9, 10]. In the current abstract we focus in a Taurid fireball named SPMN 201112 recorded on November 20 th , 2012 at 2h16m15.6s UT

Study of Mass Oxygen Transfer in a Biotrickling Filter for Air Pollution Control

Biotrickling filtration is a potential and cost effective alternative for the treatment of volatile organic compound (VOC) emissions in air, so it is necessary to deepen into the key aspects of design and operation for the optimization of this technology. One of these factors is the oxygen mass transfer of the process. This study would facilitate the selection of the packing material and the mathematical modelling and simulation of bioreactors. Four plastic packing materials with a different specific surface area have been evaluated in terms of oxygen mass transfer. For the tested range of superficial liquid velocities, data show a relationship between the kLa and the superficial liquid velocity in all packing materials used, except for the biggest plastic rings. No significant differences in mass transfer coefficients at low liquid velocities were observed, however dependency between oxygen transfer and specific surface area increased considerably for high liquid velocities. No significant influences of the superficial air velocity were observed

On the chemical nature and orbit of meteoroids from the omicron draconid stream

The omicron Draconids were first observed by Denning in the 19th Century [1]. The activity was, however, modest, with a zenithal hourly rate (ZHR) of about 10–12. Denning [2] also reported observations in 1929 but in neither case was an orbit given, only a radiant position (RA ~271º, Dec. ~60º). However, for a considerable time after Denning’s observations, no records of any activity exist. Whether this is due to a lack of observers at the pertinent time (early July and thus close to the longest day and also close to the activity period of the delta Aquariids and observers may have preferred to study those) or an intrinsic lack of activity from the Omicron Draconids is not clear. The next record appears to be by Cook et al. [3] reporting on the work of the Harvard Meteor Project in the 1950s. In that paper they also suggested that the formation of the stream was associated with the disintegration of the nucleus of comet C/1919 Q2 Metcalf. In fact, our team recorded in 2008 a mag. -18 omicron Draconid fireball which was linked to this comet [4]. Here we present the analysis of a doublestation omicron-Draconid fireball recorded in the framework of our continuous fireball monitoring and spectroscopic campaigns in July 2007. The unique spectrum obtained for a member of this stream has provides helpful information about the chemical nature of meteoroids in the omicron-Draconid stream

The Puerto Lapice eucrite fall phenomenon

The fall of the Pu erto Lápice eucrite occurred in the afternoon of May 10, 2007, 17h57m20±2s UTC. This impressive daylight bolide was witnessed by thousands of people from Spain, and is being carefully studied in the framework of the Spanish Meteor and Fireball Network (SPMN) in a similar way that we previously did after the fall of the Villalbeto de la Peña L6 or dinary chondrite [1,2]. Unfortunately, there is no video records to our knowledge of the Puerto Lápice even t, but some eyewitnesses were able to take pictures of the persistent train from at least two different locations. Nocturn astrometric calibrations from both places have been obtained, and these data together with in situ trajectory measurements with theodolite of casual eyewitnesses have allowed to estimate the atmo spheric trajectory and the radiant with reasonable accu racy. A preliminary trajectory reconstruction by the SPMN obtained only two weeks after the event helped to recover the first meteorite specimens. The meteorite was presented on June 11, 2007 during the International Conference Meteoroids 2007 in Barcelona. In addition to the fall phenomena, the interest of this bolide lies in the eucrite nature of the recovered meteorite, that has been recently reported in the Meteoritical Bulletin [3]. Of the 200 eucrites known until 2000, only 25 correspond to observed falls, but the fall circumstances are poorly known except in few remarkable cases like e.g. Pasamonte