4-8 October 2015
Hans Harnack Haus
Europe/Berlin timezone
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Contribution List

Displaying 113 contributions out of 113
Dense, star-forming cores of molecular clouds are observed to be strongly magnetized. A realistic magnetic field of moderate strength has shown to suppress the formation of a rotationally supported disk (RSD) through magnetic braking, if the neutral gas are well-coupled to the magnetic field by Cosmic-Ray (CR) ionization. Here, we present the conditions for formation of RSDs through non-ideal MHD ... More
Presented by Mr. Bo ZHAO
Type: Poster Session: Poster Viewing
Track: Poster session
The Barnard 1 cloud is one of the highest column density regions in the Perseus molecular complex, which comprises several dense cores at different evolutionary stages of star formation. Of those, B1b has been recently found to contain two very young protostellar objects, B1b-N and B1b-S, separated by 20''. IRAM PdBI observations show the presence of slow molecular outflows arising from ... More
Presented by Dr. Nuria MARCELINO
Type: Poster Session: Poster Viewing
Track: Poster session
FU Orionis-type stars (FUors) are young stellar objects experiencing large optical outbursts due to highly enhanced accretion from the circumstellar disk onto the star. FUors are often surrounded by massive envelopes, which have a significant role in the outburst mechanism. Conversely, the subsequent eruptions might gradually clear up the obscuring envelope material and drive the protostar on its ... More
Presented by Dr. Péter ÁBRAHÁM
Type: Poster Session: Poster Viewing
Track: Poster session
Observations at mm- and sub-mm wavelengths allow us to probe the solids in the disk midplane, where the bulk of the dust is located and where planets are expected to form. The distribution of dust grain size in different regions of a protoplanetary disk is a powerful probe of the physical mechanisms related to grain growth and ultimately on how solids can overcome the various growth barriers on th ... More
Presented by Mr. Marco TAZZARI
Type: Poster Session: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM (II)
Track: Poster session
The Class 0 protostar IRAS 15398–3359 is located in the Lupus I cloud at a distance of 155 pc. The source is known to harbour a molecular outflow, but the region has not attracted much interest until recently. IRAS 15398 show interesting chemical signatures and being one of the very nearby, young outflow sources makes it an excellent target for detailed studies of the gas kinematics of different ... More
Presented by Dr. Jes Kristian JORGENSEN
Type: Poster Session: Poster Viewing
Track: Poster session
A long-standing problem of the general paradigm of low-mass star formation is the "luminosity problem": protostars are less luminous than theoretically predicted. A possible solution is that the accretion process is episodic. FU Ori-type stars (FUors) are thought to be the visible examples for objects in the high accretion state. FUors are often surrounded by massive envelopes, enabling the disk t ... More
Presented by Dr. Ágnes KÓSPÁL
Type: Contributed Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (I)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 1
Spatially resolved molecular line observations have revealed circumstellar disks in Keplerian rotation around young stellar objects with masses up to 30 $M_\odot$. Line emission observations have been crucial in identifying and characterizing these disks and have allowed us to study their dynamics. In this contribution, I will discuss their properties and evolution and compare them to the circumst ... More
Presented by Dr. Maite BELTRAN on 7 Oct 2015 at 12:00
Type: Poster Session: Poster Viewing
Track: Poster session
**Context:** Dense, cold regions where protostellar objects have not yet formed (high mass starless cores, HMSCs) are poorly characterised. However, observations of regions in this phase, before the violent feedback from massive star formation events takes hold, are crucial to characterise the initial conditions for high-mass star formation (HMSF). **Aims:** The goal of this work is to inve ... More
Presented by Dr. Siyi FENG
Type: Review talk Session: FROM CLOUDS TO DENSE CORES (I)
Track: FROM CLOUDS TO DENSE CORES 1
Recent continuum surveys of the Gould's Belt and the Milky Way have identified tens of thousands of dense cores and clumps within the Galaxy.  It is now possible to study all phases of core, clump, and filament evolution before and during star formation with statistically significant samples of objects.  Astrochemical processes on these different physical scales provide astrophysical probes ... More
Presented by Dr. Yancy SHIRLEY on 5 Oct 2015 at 09:00
Type: Poster Session: Poster Viewing
Track: Poster session
Our understanding of the initial conditions of high-mass star formation are far from complete. Molecular line observations (such as MALT90 survey) are useful tools to probe the physical and chemical conditions of these clumps (such as densities, temperatures, ages, cosmic-ray ionization rates etc.). Some of the recent studies performed detailed chemical modeling of these clumps to interpret the m ... More
Presented by Dr. Rumpa CHOUDHURY
Type: Contributed Talk Session: FROM DENSE CORES TO PROTOSTARS (I)
Track: FROM DENSE CORES TO PROTOSTARS 1
What are the basic chemical mechanisms that led atoms to molecules in star forming regions? What is the role of the pre-solar chemistry in the present chemical composition of the Solar System bodies, planets, comets, and asteroids? The molecular complexity builds up at each step of the process leading to star formation, starting from simple molecules and ending up in Complex Organic Molecules (CO ... More
Presented by Dr. Claudio CODELLA on 6 Oct 2015 at 09:50
Type: Poster Session: Poster Viewing
Track: Poster session
The first hydrostatic core, also called the first Larson core, is one of the first steps in low-mass star formation, as predicted by theory. With recent and future high performance telescopes, details of these first phases become accessible, and observations may confirm theory and even bring new challenges for theoreticians. In this context, we study from a theoretical point of view the chemical a ... More
Presented by Dr. Ugo HINCELIN
Type: Contributed Talk Session: FROM CLOUDS TO DENSE CORES (II)
Track: FROM CLOUDS TO DENSE CORES 2
The W33 complex is an ideal object to study high-mass star formation since it contains molecular clouds in different evolutionary stages within a small area on the sky. The molecular clouds in W33 are located at similar distances (~2.4 kpc) and probably contained the same birth material. Thus, a comparative chemical study of these clouds along an evolutionary sequence (from quiescent dark clouds ... More
Presented by Dr. Katharina IMMER on 5 Oct 2015 at 17:15
Type: Review talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (II)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 2
I will review recent advances in observations, models, and the laboratory, which have shed new light on the chemical evolution as a protostar evolves to form the protoplanetary disk. ALMA 'Early Science' observations have allowed an unprecedented view of the molecular gas in protostars and disks on size scales approaching those of the inner Solar System (< 50 AU). In conjunction, 'hot off the pr ... More
Presented by Dr. Catherine WALSH on 7 Oct 2015 at 14:00
Type: Contributed Talk Session: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM (I)
Track: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM 1
The formation of planetesimals requires that primordial dust grains grow from micron- to km-sized bodies. As dust grains grow, they start to decouple from the gas and drift radially towards the central star. Therefore, planetesimal formation has to happen in time-scales shorter than radial drift. One way to halt the inward drift is by developing a local maximum in the radial surface density of the ... More
Presented by Dr. Asunción FUENTE on 8 Oct 2015 at 09:50
Type: Invited Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (I)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 1
The condensation fronts (snow lines) of H2O, CO and other abundant volatiles in the midplane of a protoplanetary disk affect several aspects of planet formation. Locating the CO snow line is challenging. This has prompted an exploration of chemical signatures of CO freeze-out. We present ALMA observations of the N2H+ and DCO+ emission in protoplanetary disks and evaluate their utility as tra ... More
Presented by Dr. Chunhua QI on 7 Oct 2015 at 11:20
Type: Poster Session: Poster Viewing
Track: Poster session
In order to study the time evolution of hot cores and further stages of high-mass star forming regions, we have developed a chemical code (Saptarsy, Choudhury et al., 2015 [1]) which is currently working together with a radiative transfer code (RADMC-3D, http://www.ita.uni-heidelberg.de/~dullemond/software/radmc-3d/). Saptarsy is a gas-grain code taking into account heavy radical movements at high ... More
Presented by Gwendoline STÉPHAN
Type: Poster Session: Poster Viewing
Track: Poster session
The true 3D shapes of prestellar cores can provide useful insights about the initial conditions and the processes that regulate star formation. Unfortunately, two dimensional projections on the plane of the sky, probed by dust emission maps, can be identical for different intrinsic 3D core shapes. In lifting this shape degeneracy interstellar chemistry can be proven a useful ally. We present a sim ... More
Presented by Aris TRITSIS
Type: Invited Talk Session: FROM DENSE CORES TO PROTOSTARS (II)
Track: FROM DENSE CORES TO PROTOSTARS 2
New molecules continue to be detected in hot cores, and the ALMA telescope is likely to uncover many more over the coming years. Perhaps the most exciting detections involve highly complex molecules with structures that are new to interstellar chemical networks. How can we incorporate these molecules and structures into chemical networks to make sense of new detections? I will give a brief ove ... More
Presented by Prof. Rob GARROD on 6 Oct 2015 at 14:25
Type: Contributed Talk Session: FROM DENSE CORES TO PROTOSTARS (II)
Track: FROM DENSE CORES TO PROTOSTARS 2
Radio astronomy has been an important method for identification of molecular constituents in the interstellar medium (ISM). One way to do this is by matching microwave and millimeter wave laboratory spectra to those obtained by radio observatories. Until now, the availability of laboratory data has been sufficient to keep up with the influx of astronomical data. However, with new and upgraded obse ... More
Presented by Dr. Amanda STEBER, Mr. Ben ARENAS on 6 Oct 2015 at 17:30
Type: Poster Session: Poster Viewing
Track: Poster session
Dust evolution is an important part of advanced chemical models of protoplanetary disks. Most of dust evolution models, both standalone and incorporated into thermo-chemical codes, typically considers neutral or singly charged grains. Grain charging in protoplanetary disks and its impact on the dust growth lacks currently a detailed scientific scrutiny. In this work we consider two of the primar ... More
Presented by Dr. Vitaly AKIMKIN
Type: Contributed Talk Session: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM (I)
Track: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM 1
Being remnants of the planet formation process, debris discs consist of (invisible) planetesimals and collisionally-replenished dust. Observations from optical to submm wavelengths reveal their presence around at least 20% of main-sequence stars. Systems that are spatially resolved at multiple wavelengths and have densely sampled SEDs allow us to more tightly constrain the physical properties of d ... More
Presented by Mr. Christian SCHÜPPLER on 8 Oct 2015 at 11:45
Type: Aperitif talk
Presented by Prof. Ewine VAN DISHOECK on 7 Oct 2015 at 18:30
Type: Contributed Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (I)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 1
We report compact SO emission around three class 0/I protostars found as byproducts during the ALMA observations searching for Keplerian disks. The three protostars are L1527 IRS, TMC1A, and L1489 IRS in Taurus. The ALMA observations have found Keplerian disks of 50-700 AU in radius around them in C$^{18}$O ($2-1$) emission, and also have revealed that the materials surrounding the disks are accre ... More
Presented by Prof. Nagayoshi OHASHI on 7 Oct 2015 at 10:05
Type: Contributed Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (I)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 1
Complex organic molecules are fused with low-mass star-forming systems. Such species have been observed on- and off-source in hot and cold environments, respectively [e.g., 1, 4, 5]. During the formation of the star-disk system these compounds can potentially contaminate protoplanetary and proto-cometary materials with organics. In this talk, physicochemical models are presented, including wavelen ... More
Presented by Ms. Maria DROZDOVSKAYA on 7 Oct 2015 at 12:15
Type: Review talk Session: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM (II)
Track: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM 2
A review of the composition of cometary ices will be presented, including recent discoveries of complex molecules. Abundances of complex organics in comets will be compared to values measured in hot-cores and hot-corinos, and to results of chemical models of proto-planetary disks.
Presented by Dr. Dominique BOCKELEE-MORVAN on 8 Oct 2015 at 14:00
Type: Contributed Talk Session: FROM DENSE CORES TO PROTOSTARS (I)
Track: FROM DENSE CORES TO PROTOSTARS 1
An increasing number of complex organic molecules have been found in the interstellar medium, in particular in regions where new stars are being formed. While a few of these molecules have recently even been traced back to the prestellar phase in low-mass-star forming regions, the bulk of their emission in the gas phase is detected during the early accretion phase, when the newly-born protostar st ... More
Presented by Dr. Arnaud BELLOCHE on 6 Oct 2015 at 10:05
Presented by Prof. Paola CASELLI on 8 Oct 2015 at 16:15
Type: Contributed Talk Session: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM (I)
Track: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM 1
The chemical composition of exoplanets and their atmospheres is arguably the most important ingredient in determining their mass-radius relation and their atmospherics properties. The initial chemical composition of exoplanets is a consequence of their accretion history as they migrate through their natal protoplanetary disks accreting both solids and gases as they build and move through their ho ... More
Presented by Prof. Ralph PUDRITZ on 8 Oct 2015 at 12:15
Type: Poster Session: Poster Viewing
Track: Poster session
The chemical history of the interstellar gas is one major question at the crossroads of many fields of research in astrophysics and astrochemistry, in both the local and the young Universe. The chemical heritage of planetary systems is one particular instance of this problem. Isotopic ratios are usual and powerful tools to follow chemical volatile reservoirs during the evolution of the gas from ... More
Presented by Mr. Victor DE SOUZA MAGALHÃES
Type: Invited Talk Session: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM (I)
Track: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM 1
Transitional disks are protoplanetary disks with large inner holes, large enough to cause a significant drop in the SED. It has recently been shown that most if not all of the sample of isolated Herbig Ae stars have clear indications for the existence of such holes. Interestingly, most of these objects still have host dust near the sublimation zone. I will discuss mechanisms for the creation of ... More
Presented by Carsten DOMINIK on 8 Oct 2015 at 09:25
Type: Contributed Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (I)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 1
Determination of the D/H ratios is valuable for understanding the chemical and physical conditions at earlier phases of protoplanetary disks formation, in which planets formation may occur. Understanding deuterium fractionation is thus key to explain the D/H distribution pattern found in the various bodies of our solar system. To investigate the different key gas-phase deuteration pathways that ca ... More
Presented by Dr. Cecile FAVRE on 7 Oct 2015 at 11:45
Type: Contributed Talk Session: FROM CLOUDS TO DENSE CORES (II)
Track: FROM CLOUDS TO DENSE CORES 2
The simplest amino acid glycine (NH$_2$CH$_2$COOH: d$_0$-Gly) is an achiral amino acid. However, if one of the carbon-bound hydrogen is replaced with a deuterium atom, it becomes a chiral molecule (NH$_2$CHDCOOH: d$_1$-Gly). Although there have been no reports on the detection of chiral species in space, chiral glycine has a potential to be one of the primordial chiral molecules in space. We then ... More
Presented by Dr. Yasuhiro OBA on 5 Oct 2015 at 16:45
Type: Poster Session: Poster Viewing
Track: Poster session
In this work we measure the deuterium fraction towards dense cores along the filamentary structure L1495 in the Taurus molecular cloud to investigate how different environmental conditions affect the deuterium fractionation. For this study, ${\rm N_2H^+(1-0)}$ and ${\rm N_2D^+(2-1)}$ on-the-fly maps of 13 cores were used to measure the deuterium fraction and reveal the kinematics of the cores. Obs ... More
Presented by Ms. Anna PUNANOVA
Type: Contributed Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (II)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 2
Isotopic fractionation patterns is a popular tool to date Solar System and interstellar material. Nitrogen and hydrogen fractionation, i.e. the enhancement of deuterium and $^{15}$N in molecules, are both expected to be efficient at the low temperatures found in pre-stellar cores an protoplanetary disk midplanes. These enhancements can survive the warmer phases of star and planet formation, mainta ... More
Presented by Prof. Karin ÖBERG on 7 Oct 2015 at 14:50
Type: Review talk Session: FROM DENSE CORES TO PROTOSTARS (II)
Track: FROM DENSE CORES TO PROTOSTARS 2
Water and some organic molecules were found to be deuterium enriched not only toward various astronomical targets and but also in comets and meteorites. Understanding the formation processes of deuterated species may lead to know how and when those molecules are created. Although gas phase chemistry is certainly important for deuterium enrichment, the role of physicochemical processes on the grain ... More
Presented by Prof. Naoki WATANABE on 6 Oct 2015 at 14:00
Type: Poster Session: Poster Viewing
Track: Poster session
Infrared dark clouds (IRDCs), dense and dark silhouettes against bright Galactic background, are thought to be the cradles of massive star and cluster formation, being cold, dense, and massive enough to harbour massive protostars. Previous studies show great diversity of IRDCs, ranging from dense quiescent clouds on the verge of star formation to relatively evolved regi ... More
Presented by Mr. Vlas SOKOLOV
Type: Contributed Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (I)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 1
One of the key properties for understanding how disks evolve to planetary systems is their overall mass, combined with their surface density distribution. So far, virtually all disk mass determinations are based on observations of the millimeter continuum dust emission. To derive the total gas + dust disk mass from these data involves however several big assumptions. The alternative method is t ... More
Presented by Mrs. Anna MIOTELLO on 7 Oct 2015 at 09:50
Type: Contributed Talk Session: FROM CLOUDS TO DENSE CORES (I)
Track: FROM CLOUDS TO DENSE CORES 1
What are the properties of dust in the interstellar medium (ISM) and how do these properties change in the transition to denser regions? This is one of the important questions when studying the denser ISM, since dust properties influence, for example, the formation and temperature of the major molecules in molecular clouds and the grain dynamical behaviour when forming protoplanetary disks. It is ... More
Presented by Dr. Melanie KOEHLER on 5 Oct 2015 at 12:00
Type: Poster Session: Poster Viewing
Track: Poster session
Prestellar cores are collapsing objects where gravity struggles against thermal pressure and magnetic fields in order to evolve and form a protostar. Observationally, this evolution may be traced by the gas kinematics and dust properties. In this work, we present recent results toward the object FeST 1-457, an evolved starless cores in the Pipe nebula. We report APEX dust polarization data and IRA ... More
Presented by Dr. Felipe ALVES
Type: Poster Session: Poster Viewing
Track: Poster session
Dust properties are a key issue to explore the content and structure of molecular clouds. However, they remain difficult to determine because deducing their composition and size distribution from observations is a highly degenerate problem. In particular, emission alone is not able to retrieve the coldest dust (Pagani, 2015). Other information are needed and some insights come from extinction (abs ... More
Presented by Dr. Laurent PAGANI
Type: Contributed Talk Session: FROM DENSE CORES TO PROTOSTARS (I)
Track: FROM DENSE CORES TO PROTOSTARS 1
Protostars and disks are formed within infalling envelopes of molecular gas and dust. The mass infall rate sets many of the conditions for early disk evolution. High infall rates may increase the mass of the protostellar disk enough to force gravitationally instability leading to the formation of binaries or planets and to episodic accretion from the disk to the protostar. Until recently, o ... More
Presented by Dr. Amelia STUTZ on 6 Oct 2015 at 12:00
Type: Contributed Talk Session: FROM CLOUDS TO DENSE CORES (I)
Track: FROM CLOUDS TO DENSE CORES 1
Even today in our Galaxy, stars form from gas cores in a variety of environments, which may affect the properties of the resulting star and planetary systems. Here, we study the role of pressure, parameterized via ambient clump mass surface density, on protostellar evolution and appearance, focusing on low-mass Sun-like stars and considering a range of conditions from relatively low pressure filam ... More
Presented by Prof. Jonathan TAN on 5 Oct 2015 at 10:05
Type: Invited Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (I)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 1
The evolution of solids in circumstellar disks is governed by transport processes and collisional growth. These processes are in turn driven by the dynamics of the gas disk. Dust evolution is therefore not only the first step towards forming planets, it is also a powerful probe of the structure and dynamics of the gas disk. Furthermore, key volatiles such as water or CO form/freeze-out on the s ... More
Presented by Dr. Til BIRNSTIEL on 7 Oct 2015 at 09:25
Type: Poster Session: Poster Viewing
Track: Poster session
By combining data in various wavelengths (IR, X-rays, Radio) we attempt to unlock the star forming properties of star clusters forming in diverse environments. Our goal is to understand those properties in the context of a) the presence or even the absence of massive stars, and b) the primordial structure of the cloud. We will put into consideration the possibility that the primordial structure o ... More
Presented by Dr. Carlos ROMÁN-ZÚÑIGA
Type: Aperitif talk
Presented by Dr. Christiane HELLING on 8 Oct 2015 at 17:30
Type: Contributed Talk Session: FROM DENSE CORES TO PROTOSTARS (I)
Track: FROM DENSE CORES TO PROTOSTARS 1
The origin and history of prebiotic chemistry in protostars and protoplanetary disks is a main research theme within astrochemistry. With current observational facilities it is becoming possible to routinely detect complex organic molecular species, and also to study their spatial distribution and relative abundances throughout protostellar envelopes and embedded protoplanetary disks. We will show ... More
Presented by Dr. Matthijs VAN DER WIEL on 6 Oct 2015 at 12:15
Type: Poster Session: Poster Viewing
Track: Poster session
Formamide has been detected a long time ago in the direction of Sgr B2 [2]. A systematic search of this molecule has been recently achieved with the IRAM 30-m telescope [6]. In that study formamide was detected in five (IRAS 4A, IRAS 16293, SVS13A, Cep E, and OMC-2) objects, while it was not detected in other colder sources devoid of hot corinos [1]. This was explained by invoking that NH2CHO (i) ... More
Presented by Dr. Dimitrios SKOUTERIS
Type: Contributed Talk Session: FROM DENSE CORES TO PROTOSTARS (II)
Track: FROM DENSE CORES TO PROTOSTARS 2
During the formation of stars, the accretion of the surrounding material toward the central object is thought to undergo frequent and strong eruptive outbursts, followed by long periods of relative quiescence. Such episodic events have been invoked to resolve the “luminosity problem” whereby the observed luminosity of most low-mass protostars is lower than the accretion luminosity expected fro ... More
Presented by Dr. Vianney TAQUET on 6 Oct 2015 at 14:50
Type: Poster Session: Poster Viewing
Track: Poster session
We present the results of chemical modeling of the formation of terrestrial-type complex organic molecules (COMs) under conditions typical for prestellar cores. We utilized an advanced gas-grain astrochemical model with multilayer approach to ice-surface chemistry and up-to-date treatment of reactive desorption based on recent experiments of Minissale et al. (submitted). Chemical network in the mo ... More
Presented by Dr. Anton VASYUNIN
Type: Review talk Session: FROM CLOUDS TO DENSE CORES (II)
Track: FROM CLOUDS TO DENSE CORES 2
A large fraction of molecules have been observed in cold dark sources. These astronomical objects represent the starting point for the formation of molecules that will participate in the chemistry of the birth of stars and planets. They are also supposed to be the most simple objects in term of physical conditions and history. In this review talk, we will present a summary of the recent model deve ... More
Presented by Dr. Valentine WAKELAM on 5 Oct 2015 at 14:00
Type: Invited Talk Session: FROM CLOUDS TO DENSE CORES (II)
Track: FROM CLOUDS TO DENSE CORES 2
Relatively complex organic molecules (COMs), such as formamide or cyanomethanimine, have been detected in the gas-phase of various regions of the interstellar medium. Some difficulties in assessing their formation routes under the harsh conditions of interstellar objects have progressively brought the current astrochemical models to privilege grain-surface over gas-phase chemistry to explain their ... More
Presented by Prof. Nadia BALUCANI on 5 Oct 2015 at 16:20
Type: Poster Session: Poster Viewing
Track: Poster session
We have identified a new externally irradiated Herbig-Haro (HH) jet, HH 1158, within ~2 pc of the massive OB type stars in the sigma Orionis cluster. At an Lbol ~ 0.1 Lsun, HH 1158 is the lowest luminosity irradiated HH jet source identified to date in any cluster/region. The external radiation field has improved the visibility both close to and far from the driving source, thus enabling unambiguo ... More
Presented by Dr. Basmah RIAZ
Type: Invited Talk Session: FROM CLOUDS TO DENSE CORES (II)
Track: FROM CLOUDS TO DENSE CORES 2
Molecular ions are important constituents of the interstellar medium. They are major drivers of the chemistry particularly in cold and dense molecular clouds, which are sites of star formation, and are tracers of the physical and chemical conditions in these environments. Their identification in space relies on accurately known transition frequencies provided by laboratory spectroscopy. Convention ... More
Presented by Dr. Sandra BRÜNKEN on 5 Oct 2015 at 14:25
Type: Contributed Talk Session: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM (I)
Track: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM 1
The minimum size of dust grains in debris discs is a sensitive indicator of a variety of physical processes operating in these systems. We analysed a sample of 32 Herschel-resolved debris discs to derive the minimum grain size and found an intriguing trend of that size changing with the luminosity of the debris disc host star. The trend is statistically significant and is pretty robust against v ... More
Presented by Ms. Nicole PAWELLEK on 8 Oct 2015 at 10:05
Type: Contributed Talk Session: FROM DENSE CORES TO PROTOSTARS (I)
Track: FROM DENSE CORES TO PROTOSTARS 1
The two stable less abundant isotopes of hydrogen and nitrogen, D and 15N, are both enriched in comets and carbonaceous chondrites with respect to the values measured in the proto-solar nebula. This raises the question whether the two enrichments have a common origin, and how both are linked to the past chemical history of the Solar System. I will present new low-angular resolution observations of ... More
Presented by Dr. Francesco FONTANI on 6 Oct 2015 at 12:30
Type: Poster Session: Poster Viewing
Track: Poster session
IRAS16293E is a prestellar core located in the vicinity of a well-known multiple class 0 system and a lesser known class I object. The west side of the core is heated by the protostars, mostly via the mechanical interaction of their outflows. Previous studies have revealed a strong DCO$^+$ peak, a ND$_3$ peak and a dust peak, all misaligned. Strong H$_2$D$^+$ and a tentative detection of D$_2$H$^ ... More
Presented by Dr. Laurent PAGANI
Type: Contributed Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (II)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 2
The internal physical and chemical structure of protoplanetary disks is of fundamental importance to understand how planets form. To infer this structure from observations, new 'holistic' disk models have been developed in the frame of the EU FP7 project *DIANA* which include detailed 2D dust and PAH radiative transfer, thermo-chemical gas and ice modeling, and 3D diagnostic radiative transfer to ... More
Presented by Dr. Peter WOITKE on 7 Oct 2015 at 17:00
Type: Contributed Talk Session: FROM CLOUDS TO DENSE CORES (I)
Track: FROM CLOUDS TO DENSE CORES 1
The problem of impulsive heating of dust grains in cold, dense interstellar clouds is revisited theoretically, with the aim to better understand leading mechanisms of the explosive desorption of icy mantles. It is rigorously shown that if the heating of a reactive medium occurs within a sufficiently localized spot (e.g., heating of mantles by cosmic rays), then the subsequent thermal evolutio ... More
Presented by Dr. Alexei IVLEV on 5 Oct 2015 at 12:15
Type: Contributed Talk Session: FROM DENSE CORES TO PROTOSTARS (II)
Track: FROM DENSE CORES TO PROTOSTARS 2
It is largely accepted that Galactic cosmic rays, which pervade the interstellar medium, originate by means of shock waves in supernova remnants [1]. Cosmic rays activate the rich chemistry that is observed in a molecular cloud [2] and they also regulate its collapse timescale [3], determining the efficiency of star and planet formation, but they cannot penetrate up to the densest part of a molecu ... More
Presented by Dr. Marco PADOVANI on 6 Oct 2015 at 17:00
Type: Poster Session: Poster Viewing
Track: Poster session
This study reports the first extensive investigation of the relationship; enthalpy of formation, stability and abundance (ESA) existing among interstellar molecules using high level quantum chemical calculations. Hundreds of molecules comprising of different isomeric groups, several interstellar carbon chains and various protonated species have been considered. From the results, it is evident that ... More
Presented by Mr. emmanuel ETIM
Type: Poster Session: Poster Viewing
Track: Poster session
The components of the interstellar medium (ISM) are continuously heated due to energy input from different sources, one being the radiation of young and massive stars. In photon-dominated regions (PDRs) the interstellar far-ultraviolet (FUV; 6-13.6 eV) radiation field determines the energy balance and the chemistry of the ISM. Cooling of the gas in PDRs is dominated by fine structure lin ... More
Presented by Mrs. Silke ANDREE-LABSCH
Type: Poster Session: Poster Viewing
Track: Poster session
We present NH$_3$ and CCS observations of the L1495-B218 filaments in the Taurus molecular cloud covering over a 3 degree angular range using the K-band focal plane array on the 100m Green Bank Telescope. The L1495-B218 filaments form an interconnected, nearby, large complex extending over 8 pc. We observed NH$_3$ (1,1) \& (2,2) and CCS 2$_1$ $-$ 1$_2$ with a spectral resolution of 0.038 km/s and ... More
Presented by Mr. Youngmin SEO
Type: Invited Talk Session: FROM DENSE CORES TO PROTOSTARS (II)
Track: FROM DENSE CORES TO PROTOSTARS 2
My talk will review the most recent laboratory work performed at the Sackler Laboratory for Astrophysics (Leiden University, NL), at the Blake Research Group (Caltech, US), and at the Astrochemistry Group (Open University, UK). Laboratory experiments showed that surface reaction mechanisms on cold interstellar dust grains initiate molecular chemistry through the formation of H2, and likely dominat ... More
Presented by Dr. Sergio IOPPOLO on 6 Oct 2015 at 16:20
Type: Contributed Talk Session: FROM DENSE CORES TO PROTOSTARS (II)
Track: FROM DENSE CORES TO PROTOSTARS 2
Aromatic hydrocarbon is one of the main component of interstellar and circumstellar dust. The hydrogenation and deuteration of interstellar aromatic hydrocarbons is of particular interest for the formation of aliphatic hydrocarbons and their deuterated isotopologues. Here, we investigated the hydrogenation/deuteration reactions of amorphous solid benzene (C6H6) at low temperatures of 10–50 K. ... More
Presented by Dr. Tetsuya HAMA on 6 Oct 2015 at 15:05
Type: Poster Session: Poster Viewing
Track: Poster session
The formation of high-mass stars is one of the major topics of astrophysical research, in particular the process of accretion from large-scale clouds (a few 10 pc) down to small-scale cores (a few 0.01 pc). We have selected the nearby high-mass star forming complex NGC6334 to study the gas velocities at different scales and probe the infall rates onto the protostellar cores embedded in the mo ... More
Presented by Dr. Alvaro SANCHEZ-MONGE
Type: Contributed Talk Session: FROM CLOUDS TO DENSE CORES (I)
Track: FROM CLOUDS TO DENSE CORES 1
In the past decades more and more elaborated chemical networks have been developed to describe the chemical conditions of star forming regions under various conditions. However, due to their complexity and high computational demands, they have mainly been applied to one-zone models or static configurations. In contrast, the application to time-dependent, magentohydrodynamical (MHD) simulations has ... More
Presented by Dr. Daniel SEIFRIED on 5 Oct 2015 at 12:30
Type: Contributed Talk Session: FROM CLOUDS TO DENSE CORES (II)
Track: FROM CLOUDS TO DENSE CORES 2
The SILCC project (SImulating the Life-Cycle of molecular Clouds, Walch et al. arXiv:1412.2749; http://hera.ph1.uni-koeln.de/~silcc/) aims at a more self-consistent understanding of the interstellar medium on small scales and its link to galaxy evolution. We simulate the evolution of the multi-phase ISM in a 500 pc x 500 pc x 10 kpc region of a galactic disc, with a gas surface density of $\Sigma_ ... More
Presented by Dr. Thomas PETERS on 5 Oct 2015 at 17:30
Type: Contributed Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (I)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 1
The Orion molecular cloud is one the more observed object in sky. Spectra at millimeter and submillimeter waves have been obtained from ground to space born platforms. Together with SgrB2 it exhibits the densest line spectrum. The identification of all these features requires devoted laboratory work to identify all lines coming from isotopologues and vibrationally excited states of abundant specie ... More
Presented by Prof. Jose CERNICHARO on 7 Oct 2015 at 12:30
Type: Invited Talk Session: FROM CLOUDS TO DENSE CORES (I)
Track: FROM CLOUDS TO DENSE CORES 1
Within the ASAI (Astrochemical Surveys At Iram) Large Program, we conducted an unbiased spectral exploration of a carefully selected sample of template sources, which cover the full formation process of solar-type stars to understand the chemical evolution of the matter during the long process that brought it from prestellar cores and protostars to protoplanetary disks, and ultimately to the bodie ... More
Presented by Dr. Charlotte VASTEL on 5 Oct 2015 at 11:20
Type: Invited Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (II)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 2
The synthesis of molecules is a long and convoluted process. The molecular universe begins at the border of molecular clouds, and chemical complexity increases throughout the star formation process (Caselli & Ceccarelli 2012). Interstellar dust grains play many roles in the evolution of clouds, stars and planets, and among them, grains are effective catalytic centers, sometimes called chemical ... More
Presented by Prof. Francois DULIEU on 7 Oct 2015 at 14:25
Type: Poster Session: Poster Viewing
Track: Poster session
In dense and cold molecular clouds dust grains are surrounded by thick icy mantles. It is however not clear if dust growth and coagulation take place before star formation begins. This is an important issue, as the presence of large grains may affect the chemical structure of dense cloud cores, including the dynamically important ionisation fraction, and the future evolution of solids in protoplan ... More
Presented by Mrs. Ana CHACON-TANARRO
Type: Poster Session: Poster Viewing
Track: Poster session
The initial multiplicity of stellar systems is highly uncertain, but it provides an important constrain to the understanding of star formation. A number of mechanisms have been proposed to explain the origin of binary and multiple star systems, including core fragmentation, disk fragmentation and stellar capture. Observations show that protostellar and pre-main-sequence multiplicity is higher than ... More
Presented by Dr. Jaime PINEDA
Type: Poster Session: Poster Viewing
Track: Poster session
Despite being one of the most abundant elements in the universe, the interstellar chemistry of sulfur remains relatively poorly understood. It is known to be depleted during the early evolution of interstellar clouds, but the exact forms in which it may be found is far from certain. In the hopes of shedding some light on the question of sulfur depletion, we have significantly expanded the gas/grai ... More
Presented by Dr. Jacob LAAS
Type: Invited Talk Session: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM (I)
Track: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM 1
A growing number of main sequence stars show evidence for circumstellar gas. It is most often CO that is detected, which is puzzling because this molecule should have a short lifetime due to photo-dissocation by the interstellar radiation field. Since this gas is usually found around young stars, the most obvious explanation would be that this is a remnant of the primordial protoplanetary disk tha ... More
Presented by Dr. Mark WYATT on 8 Oct 2015 at 11:20
Type: Invited Talk Session: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM (II)
Track: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM 2
Comet 67P/Churyumov-Gerasimenko (67P) is a Jupiter Family comet targeted by the Rosetta mission for in-situ analysis of cometary material and properties. The ROSINA (Rosetta Orbiter Sensor for Ion and Neutral Analysis) instrument on board of the Rosetta spacecraft has been analyzing the composition of gases emitted from 67P since August, 2014 [1]. Here we review the different molecular and isotopi ... More
Presented by Prof. Olivier MOUSIS on 8 Oct 2015 at 15:05
on 8 Oct 2015 at 16:45
Type: Contributed Talk Session: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM (I)
Track: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM 1
In this talk, we will present a new model for time evolving accretion discs (Bitsch et al. 2015) and its influence on the formation of planetary cores via pebble accretion and on the formation of gas giants in these discs (Bitsch et al. 2015b, in review). We will also show the influence of the ice to silicate ratio on the structure of the protoplanetary disc and hence on planet formation (Bitsch e ... More
Presented by Dr. Bertram BITSCH on 8 Oct 2015 at 12:00
Type: Contributed Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (II)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 2
We present our new ALMA observations of $^{13}$CO and C$^{18}$O 6-5 in TW Hya. These data include the first direct detection of the CO snow line in this system and exciting evidence of non-Keplarian structure in the inner 20 AU. Snow lines represent volatile sublimation fronts in protoplanetary disks, which are believed to aid in the growth of planetesimals. In this regard the $^{13}$CO 6-5 image ... More
Presented by Ms. Kamber SCHWARZ on 7 Oct 2015 at 17:30
Type: Contributed Talk Session: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM (II)
Track: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM 2
Identifying the formation history of the solar system's water and simple organic content is central to understanding the conditions that fostered life in at least one planetary system, and how common such conditions are elsewhere. A key clue in this pursuit is that both water and organics in primitive solar system bodies are characteristically enhanced in their deuterated isotopologue relative to ... More
Presented by Dr. L. Ilsedore CLEEVES on 8 Oct 2015 at 14:50
Type: Aperitif talk
Presented by Prof. Hans ZINNECKER on 6 Oct 2015 at 18:30
Type: Poster Session: Poster Viewing
Track: Poster session
Using a novel combination of submillimeter dust emission maps from both Herschel and APEX-Laboca and near-infrared dust extinction measurements, we constrain the dust opacity in starless cores in the Pipe Nebula. Such observations are particularly interesting because they can directly yield signatures of dust grain growth. In the first step, we use a combination of dust emission and extinction mea ... More
Presented by Jan FORBRICH
Type: Contributed Talk Session: FROM CLOUDS TO DENSE CORES (II)
Track: FROM CLOUDS TO DENSE CORES 2
We report on a new gas-grain chemistry model (Sipilä et al. 2015b) that contains multiply deuterated species and separates out the different nuclear spin isomers of molecules with several H and/or D nuclei. The nuclear spin branching ratios are calculated using symmetry rules under the assumption of complete scrambling. The method has been previously used for systems consisting of five H and/or D ... More
Presented by Dr. Olli SIPILÄ on 5 Oct 2015 at 14:50
Type: Poster Session: Poster Viewing
Track: Poster session
The Car I photodissociation region (PDR) in NGC 3372 is illuminated by dozens of OB stars belonging to the massive open cluster Trumpler 14, whose nucleus is located at a projected distance of approximately 6 arcmin (4.5 pc) from its borders. We present the observed properties of the PDR as well as those of the very young stellar population embedded in it. These are based on ground-based op ... More
Presented by Dr. Mauricio TAPIA
Type: Contributed Talk Session: FROM CLOUDS TO DENSE CORES (II)
Track: FROM CLOUDS TO DENSE CORES 2
Observations of star-forming sites rely heavily on the use of molecular tracers. However, the abundance of these tracers is not constant: it is a result of a complex network of chemical reactions, and it depends on the age, density, and dynamical history of the star-forming site. This chemical lens can introduce distortions in our observational understanding of star formation. In this talk, I w ... More
Presented by Prof. Konstantinos TASSIS on 5 Oct 2015 at 17:00
Type: Contributed Talk Session: FROM DENSE CORES TO PROTOSTARS (I)
Track: FROM DENSE CORES TO PROTOSTARS 1
While there have been numerous studies of the disk and jet chemistry in evolved T Tauri stars, observations of the jet-disk system in protostars are very difficult due to their embedded nature and to the occurrence of numerous other kinematical components in the circumstellar region (cavities of swept-up material, infalling envelope, static ambient cloud). I will show how to exploit the combina ... More
Presented by Dr. Linda PODIO on 6 Oct 2015 at 11:45
Type: Poster Session: Poster Viewing
Track: Poster session
Using density functional theory methods we studied several molecules that could help in the solution of the missing sulphur problem in dense clouds and circumstellar regions, as well as in the clarification of the sulphur chemistry in comets. We calculated infrared spectra of the following molecules: the trimer (CH$_2$S)$_3$ and the tetramer (CH$_2$S)$_4$ of thioformaldehyde, pentathian S$_5$CH$_ ... More
Presented by Prof. Goranka BILALBEGOVIC
Type: Contributed Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (II)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 2
The total gas mass of a protoplanetary disk is a fundamental, but poorly determined, quantity. A new technique (Bergin et al. 2013) has been demonstrated to assess directly the bulk molecular gas reservoir of molecular hydrogen using the HD J=1-0 line at 112 microns. In this work we present a survey of T Tauri disk observations of the HD line. Line emission is detected in two cases at >3 sigma si ... More
Presented by Dr. Melissa MCCLURE on 7 Oct 2015 at 15:05
Type: Contributed Talk Session: FROM CLOUDS TO DENSE CORES (II)
Track: FROM CLOUDS TO DENSE CORES 2
Initial conditions are crucial to understanding the formation of massive stars, which is still a mystery. One of the most debated points is whether massive star formation is a fast or slow process. Tan et al. (2013, ApJ, 779, 96, hereafter T13) discovered two massive starless cores C1-N and C1-S with ALMA. Their study suggests $\sim$mG magnetic field be present if the cores are virialized. ... More
Presented by Shuo KONG on 5 Oct 2015 at 15:05
Type: Poster Session: Poster Viewing
Track: Poster session
In the local universe, star formation occurs entirely in molecular clouds: the densest and coldest phase of the interstellar medium (ISM). Research into the astrochemical evolution of molecular clouds is essential to understand molecular cloud observations from theory. Molecular cloud observations show that different molecules are sensitive to different physical parameters, especially temperature ... More
Presented by Mr. Brandt GACHES
Type: Invited Talk Session: FROM CLOUDS TO DENSE CORES (I)
Track: FROM CLOUDS TO DENSE CORES 1
Observations at mid-IR and far-IR wavelengths have revealed that the ISM in our Galaxy is highly organised in cold and dense filamentary structures. The most massive of these structures are called Infrared-Dark Clouds (or IRDCs) and are believed to be the initial conditions of massive star and star cluster formation. In the past decade, a large effort has been made to determine the global physical ... More
Presented by Dr. Izaskun JIMENEZ-SERRA on 5 Oct 2015 at 09:25
Type: Review talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (I)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 1
In this talk I will review our current, and evolving, understanding of the physics and chemistry of gas rich disks, including the youngest stages as the disk is forming. The record of the earliest stages of disk formation is only now being constrained and it is an open question as how much of the initial chemical composition is altered during this stage. In this light, I will discuss key ... More
Presented by Prof. Edwin BERGIN on 7 Oct 2015 at 09:00
Type: Invited Talk Session: FROM DENSE CORES TO PROTOSTARS (I)
Track: FROM DENSE CORES TO PROTOSTARS 1
The formation of disks and binary systems is thought to begin early in the star formation process. However, there have not been sufficient numbers of young protostars observed with high enough resolution to determine when and where most binaries and disks form. To significantly improve our knowledge of protostellar disks and multiplicity we have carried out the VANDAM survey, a 264 hour Jans ... More
Presented by Dr. John TOBIN on 6 Oct 2015 at 11:20
Type: Poster Session: Poster Viewing
Track: Poster session
We present the first results from the Large Program ‘ASAI’ (A Chemical Survey of Sun-like Starforming Regions) which is being carried out with the IRAM 30-m radio telescope. The project consists of high-sensitivity systematic spectral line surveys (in the wavelength ranges around 1, 2, and 3 mm) of 10 targets at different stages of the early protostellar evolution. This allows a detailed st ... More
Presented by Dr. Charlotte VASTEL
Type: Invited Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (II)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 2
In the interstellar medium (ISM), amorphous silicates and carbonaceous materials must be the result of grain condensation and growth at low temperatures and densities in molecular clouds. In our laboratory, we have designed experiments to study the cold condensation and processing of silicates and carbon material in the ISM. Molecular precursors that are the results of destructive dust processes ... More
Presented by Cornelia JÄGER on 7 Oct 2015 at 16:20
Type: Poster Session: Poster Viewing
Track: Poster session
While detailed studies of protoplanetary disk structure around low-mass stars are state of the art, few spatially resolved observations exist for high-mass objects, but come into reach with the recent advances in sub-/mm interferometers. AFGL490 is an example of an YSO at the border between intermediate and high mass with a circumstellar disk previously resolved in $\mathrm{C^{17}O}$. We ... More
Presented by Dr. Claudia MARKA
Type: Contributed Talk Session: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM (II)
Track: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM 2
The Solar System is the result of a long and complex process that transformed an initial diffuse cloud of the interstellar medium into planets, asteroids and comets. Like in the Grimm’s tale, we can find some crumbs, left along the process, which can help us to understand the path that lead where we are today. Among them, the short lived radionuclides decay products in meteoritic and terrestrial ... More
Presented by Prof. Cecilia CECCARELLI on 8 Oct 2015 at 15:30
Type: Contributed Talk Session: FROM CLOUDS TO DENSE CORES (I)
Track: FROM CLOUDS TO DENSE CORES 1
The Barnard 1b core in the Perseus molecular cloud is remarkable in several aspects : *i)* It hosts three protostars, including two class 0 sources and a more evolved object. One of the class 0 sources is very young and could still be at the first hydrostatic core stage. *ii)* The core is magnetized with a ratio $\mu$ of mass to flux to critical mass to flux between 2 and 10. Protostellar ... More
Presented by Prof. Maryvonne GERIN on 5 Oct 2015 at 11:45
Type: Poster Session: Poster Viewing
Track: Poster session
The cyclic C$_3$H$_2$ is the most stable isomer of the C$_3$H$_2$ system. It has been detected in space 30 years ago together with its singly deuterated isotopologue, $c$-C$_3$HD (Thaddeus et al., 1985 and Bell et al., 1988). The doubly deuterated $c$-C$_3$H$_2$, $c$-C$_3$D$_2$, was detected very recently in space for the first time, in L1544 and TMC-1C (Spezzano et al., 2013), and in L1527 (Tokud ... More
Presented by Dr. Silvia SPEZZANO
Type: Poster Session: Poster Viewing
Track: Poster session
How do planets form in accretion disks? What is the origin of structure leading to planet formation? One possibility, but not the only possibility, is gravitational fragmentation of an unstable disk. Under what conditions does this take place? Do all disks fragment? The current observational state of the art for low-mass stellar systems is represented by recent ALMA, Subaru, VLTI, and VLA obse ... More
Presented by Dr. Eric KETO
Type: Poster Session: Poster Viewing
Track: Poster session
We present thermochemical models of the density and temperature struture of the disk around the transition object, DM Tau. DM Tau is an accreting, low mass T Tauri star with a relatively low X-ray luminosity, the disk is inferred to have an inner $\sim 3-15$AU dust hole and a large radial extent($\sim$ 800 AU). The DM Tau disk is believed to be at a late stage of evolution, perhaps with ongoing pl ... More
Presented by Uma GORTI
Type: Contributed Talk Session: FROM DENSE CORES TO PROTOSTARS (II)
Track: FROM DENSE CORES TO PROTOSTARS 2
The understanding of hydrogen attachment to carbonaceous surfaces is essential to a wide variety of research fields and technologies such as hydrogen storage for transportation but also for the formation of cosmic H2 and the identification of stable PAHs in space. For coronene cations as prototypical Polycyclic Aromatic Hydrocarbon (PAH), the existence of magic numbers upon hydrogenation was unc ... More
Presented by Ms. stephanie CAZAUX on 6 Oct 2015 at 16:45
Type: Poster Session: Poster Viewing
Track: Poster session
Water is a crucial molecule in the physics and chemistry of star- and planet formation, but its evolution from cold cores to disks is still poorly constrained. The gas-phase abundance of water varies between cold and warm regions up to a factor of $10^{5}$ and this abundance variation makes water an excellent diagnostic of the physical structure in these sources. The origin of the warm water emi ... More
Presented by Dr. John TOBIN
Type: Contributed Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (II)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 2
The formation of many saturated species that have been observed in a wide variety of astronomical objects cannot be explained by gas phase chemistry alone and it is clear that surface chemistry must play a crucial role. Most of this chemistry occurs through a diffusive mechanism. Gas-grain models which include this type of chemistry, use however many assumptions on input parameters such as diffusi ... More
Presented by Dr. Herma CUPPEN on 7 Oct 2015 at 16:45
Type: Review talk Session: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM (I)
Track: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM 1
I will discuss new results on the formation of planets and the role of ice lines in planet formation. Pebbles play a crucial role both for the formation of planetesimals by particle concentration followed by gravitational collapse and for the subsequent rapid growth of planets by pebble accretion. The chemical composition of the pebbles depends strongly on the local temperature of the protopl ... More
Presented by Dr. Anders JOHANSEN on 8 Oct 2015 at 09:00
Type: Invited Talk Session: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM (II)
Track: PROTOPLANETARY DISK EVOLUTION AND SOLAR SYSTEM 2
Comets are believed to belong to the most pristine bodies in the solar system. The study of their composition can therefore give us important clues about the processes that occurred during the solar system formation [1]. The composition of cometary atmospheres has been investigated remotely and by in situ spacecraft measurements. Until now more than twenty molecules have been identified [2]. ... More
Presented by Léna LE ROY on 8 Oct 2015 at 14:25
Type: Review talk Session: FROM DENSE CORES TO PROTOSTARS (I)
Track: FROM DENSE CORES TO PROTOSTARS 1
Protostars in their earliest, deeply embedded, stages provide an important astrochemical laboratory, serving as the evolutionary link between dense regions in molecular clouds and the end-products in terms of the emerging protoplanetary disks. In recent years significant progress has been made on understanding the physical and chemical evolution of young stars during through stages. In particular, ... More
Presented by Dr. Jes Kristian JORGENSEN on 6 Oct 2015 at 09:00
Type: Contributed Talk Session: FROM PROTOSTARS TO PROTOPLANETARY DISKS (II)
Track: FROM PROTOSTARS TO PROTOPLANETARY DISKS 2
The volatile elements hydrogen, nitrogen, and oxygen show large isotopic variations among the solar system bodies. These isotopic heterogeneities are peculiar, because the isotopic composition of solar system matter is generally quite homogeneous. Thus, understanding the origin of the volatile stable isotope anomalies will contribute substantially to our understanding when and where the different ... More
Presented by Dr. Susanne WAMPFLER on 7 Oct 2015 at 17:15
Type: Contributed Talk Session: FROM DENSE CORES TO PROTOSTARS (II)
Track: FROM DENSE CORES TO PROTOSTARS 2
The increasing number of detections of complex organic molecules around young stellar objects strongly suggests that they are part of the material of which planetary systems are made of. These molecules play a central role in interstellar prebiotic chemistry and may be directly linked to the origin of life. Since the hot and dense molecular cores surrounding massive stars harbor the richest chemis ... More
Presented by Dr. Victor Manuel RIVILLA on 6 Oct 2015 at 17:15
Type: Invited Talk Session: FROM DENSE CORES TO PROTOSTARS (I)
Track: FROM DENSE CORES TO PROTOSTARS 1
One of the major questions regarding the origin of life on Earth is whether the original mechanism that led from simple molecules to life was connected to metabolism or to genetics, both intimately linked in living beings. Formamide (NH$_2$CHO) contains the four most important elements for biological systems, and it has recently been proposed as a precursor of both metabolic and genetic material, ... More
Presented by Dr. Ana LOPEZ-SEPULCRE on 6 Oct 2015 at 09:25
Type: Contributed Talk Session: FROM CLOUDS TO DENSE CORES (I)
Track: FROM CLOUDS TO DENSE CORES 1
Filaments are ubiquitous structures in star-forming complexes, which often intersect in high-density regions associated with star formation, know as hub-filament systems. Despite filaments having been recognized more than 30 years ago, the ubiquity of such structures in star-forming regions, which has been recently highlighted by Herschel programs, has brought special attention to their formation ... More
Presented by Dr. Gemma BUSQUET on 5 Oct 2015 at 09:50
Type: Aperitif talk
Presented by Dr. Leonardo TESTI on 5 Oct 2015 at 18:30
Type: Poster Session: Poster Viewing
Track: Poster session
Water is a fundamental molecule for the physical and chemical evolution of proto-stellar and proto-planetary systems and eventually for the fomation of planetary atmospheres. Spitzer observations have revealed a high abundance of water in the inner region of protoplanetary disks. Most recent observations with Herschel shed light on the water content in the outer, cold, disk reservoir. The re ... More
Presented by Davide FEDELE