scholarly journals Direct Imaging of Bridged Twin Protoplanetary Disks in a Young Multiple Star

2011 ◽  
Vol 7 (S282) ◽  
pp. 425-428
Author(s):  
Satoshi Mayama ◽  
Motohide Tamura ◽  
Tomoyuki Hanawa ◽  
Tomoaki Matsumoto ◽  
Miki Ishii ◽  
...  
Keyword(s):  
Binary System ◽  
Binary Systems ◽  
Planet Formation ◽  
Protoplanetary Disks ◽  
Theoretical Models ◽  
Direct Image ◽  
Great Opportunity ◽  
Multiple Star ◽  
Multiple Systems ◽  
Spiral Arm

AbstractProtoplanetary disks are ubiquitously observed around young solar-mass stars and are considered to be not only natural by-products of stellar evolution but also precursors of planet formation. If a forming star has close companions, the protoplanetary disk may be seriously influenced. It is important to consider this effect because most stars form as multiples. Thus, studies of protoplanetary disks in multiple systems are essential to describe the general processes of star and planet formation.We present the direct image of an interacting binary protoplanetary system. We obtained an infrared image of a young multiple circumstellar disk system, SR24, with the Subaru 8.2-m Telescope. Both circumprimary and circumsecondary disks are clearly resolved with a 0.1 arcsecond resolution. The binary system exhibits a bridge of infrared emission connecting the two disks and a long spiral arm extending from the circumprimary disk. A spiral arm would suggest that the SR24 system rotates counter-clockwise. The orbital period of the binary is 15,000 yr. Numerical simulations reveal that the bridge corresponds to gas flow and a shock wave caused by the collision of gas rotating around the primary and secondary stars. The simulations also show that fresh material streams along the spiral arm, confirming the theoretical proposal that gas is replenished from a circum-multiple reservoir. These results reveal the mechanism of interacting protoplanetary disks in young multiple systems. Furthermore, our observations provide the first direct image that enables a comparison with theoretical models of mass accretion in binary systems. The observations of this binary system provide a great opportunity to test and refine theoretical models of star and planet formation in binary systems.

Exploring the dust ring in the circum-binary disc around GG Tau A

2021 ◽  
Author(s):  
Claudia Toci ◽  
Simone Ceppi ◽  
Nicolas Cuello ◽  
Giuseppe Lodato ◽  
Cristiano Longarini ◽  
...  
Keyword(s):  
Binary Systems ◽  
Planet Formation ◽  
Initial Conditions ◽  
Scattered Light ◽  
Complex Structure ◽  
Semimajor Axis ◽  
Continuum Emission ◽  
Orbital Parameter ◽  
Semi Major Axis ◽  
Multiple Systems

<p>Binaries and multiple systems are common among young stars (Reipurth et al. 2014). These stars are often surrounded by discs of gas and dust, formed due to the conservation of angular momentum of the collapsing cloud, thought to be the site of planet formation.<br />In the case of binary systems, three discs can form: an outer disc surrounding all the stars (called circumbinary disc), and two inner discs around the stars. As circumbinary planets have recently been discovered by Kepler (see e.g., Martin 2018, Bonavita & Desidera 2020), it is crucial to understand the dynamics and evolution of circumbinary discs to better understand the initial conditions of planet formation in multiple systems.<br />The GG Tau A system is an example of a young multiple T Tauri star. The binary is surrounded by a bright disc, observed in the continuum emission at different wavelengths (see e.g., Guilloteau et al. 1999; Dutrey et al. 2014; Phuong et al. 2020b) and in scattered light (e.g., Duchene et al. 2014, Keppler et al. 2020). The disc extends in the dust from 180 to 280 au from the center of mass, and in the gas up to 850 au. The inner (<180 au) part is depleted in gas and dust. Scattered light images show a complex structure in the inner part of the disc, with arcs and filamentary structures connecting the outer ring with the arcs and three shadows.<br />Two different configurations are possible fitting the proper motion data for the system: a co-planar case with a low eccentricity binary with a semi-major axis of 34 au, explored by Cazzoletti et al. 2017 and Keppler et al. 2020, and a misaligned case (i=30) with an eccentric binary (e=0.45) and a wider semimajor axis of 60 au (Aly et al.2018). At the state of the art, all these analyses focused on the gas dynamics only.<br />We will show the results of new 3D SPH simulations of dust and gas performed with the code PHANTOM, devised to test the two possible scenarios. We will describe the dynamics of the system in the two cases, comparing our models with observational results in order to better constraint the orbital parameter of the GG Tau A system. Our predictions will guide future observing campaigns and shed light on the complex evolution of discs in triple stellar systems.</p> <p> </p>

Dust Particle Settling in Protoplanetary Disks around Young Stars in Binary Systems

2004 ◽  
Vol 202 ◽  
pp. 365-367
Author(s):  
Y. Sato ◽  
Y. Nakagawa
Keyword(s):  
Dust Particle ◽  
Binary Systems ◽  
Protoplanetary Disks ◽  
Young Stars ◽  
Close Binary ◽  
Dust Particles ◽  
Gravitational Perturbation ◽  
Particle Settling ◽  
Multiple Systems ◽  
Close Binary Systems

We calculate the SEDs of young stars accompanied by protoplanetary disks, taking into account the effect of the settling of dust particles. Observed disk candidates contain significant number of binary or multiple systems. We compare our results with observed data and obtain many excellent fittings. From the results, it is found that in close binary systems the disk masses are relatively low and dust particles is hard to settle as compared with the cases of disks in wide binaries or around isolated stars. This is attributable to gravitational perturbation from the companion stars, which will disturb formation of planetary systems in close binary systems.

scholarly journals Direct imaging of bridged twin protoplanetary disks in a young multiple star

2010 ◽  
Vol 6 (S276) ◽  
pp. 506-507
Author(s):  
Satoshi Mayama ◽  
Motohide Tamura ◽  
Tomoyuki Hanawa ◽  
Tomoaki Matsumoto ◽  
Miki Ishii ◽  
...  
Keyword(s):  
Shock Wave ◽  
Numerical Simulations ◽  
Gas Flow ◽  
Near Infrared ◽  
Protoplanetary Disks ◽  
Infrared Emission ◽  
Direct Imaging ◽  
Multiple Star ◽  
Fresh Material ◽  
Spiral Arm

AbstractStudies of the structure and evolution of protoplanetary disks are important for understanding star and planet formation. Here, we present the direct image of an interacting binary protoplanetary system. Both circumprimary and circumsecondary disks are resolved in the near-infrared. There is a bridge of infrared emission connecting the two disks and a long spiral arm extending from the circumprimary disk. Numerical simulations show that the bridge corresponds to gas flow and a shock wave caused by the collision of gas rotating around the primary and secondary stars. Fresh material streams along the spiral arm, consistent with the theoretical scenarios where gas is replenished from a circummultiple reservoir.

Linear and non-linear tidal oscillations and mode identification in the eccentric binary system KIC 3858884

2020 ◽  
Vol 498 (2) ◽  
pp. 1871-1890
Author(s):  
Davood Manzoori
Keyword(s):  
Binary System ◽  
Binary Systems ◽  
Theoretical Models ◽  
High Amplitude ◽  
Relativity Theory ◽  
Geometrical Parameters ◽  
Single Star ◽  
Mode Identification ◽  
Pulsating Stars ◽  
Fourier Frequency

ABSTRACT The phoebe code was used to analyse the Kepler light-curve and to estimate the physical and geometrical parameters of a rare pulsating binary system, KIC 3858884. The analysis indicated that the system is composed of two detached and very similar main-sequence A-type stars, in a highly eccentric orbit with e = 0.47. After disentangling the binarity effect, the residual data were subjected to Fourier frequency decomposition using period04 software. The resulting frequency spectrum consists of two moderately high-amplitude nearby frequencies, F1 = 7.232199 d−1 and $F2=7.472889\, \mathrm{d}^{-1}$, which were attributed to δ Scuti-type pulsations. In addition, 18 frequencies were identified that were exact harmonics of the orbital frequency $f_{\rm orb}= 0.038533\, \mathrm{d}^{-1}$, and also 53 anharmonics. However, it was found that many of these anharmonic frequencies coupled together non-linearly to give harmonic modes of pulsation. Furthermore, some existing theoretical models of the tidal oscillations were numerically verified in general binary systems through estimations of various modal characteristics, for example mode quantum numbers ${n, l, m,}$ energies Ei, threshold energies Ei,th, damping rates γi, growth rates Γi and stability criteria, etc. The evolution of the stars in the binary system was compared with some similar single pulsating stars on the Hertzsprung–Russell diagram and it was concluded that the evolution of a single star is more rapid. Finally, the observed rate of apsidal line displacement was estimated through eclipse timing variation analysis as Uobs  = 74745.2 ± 2566 yr. This was compared with the theoretically calculated rate of the line of apsides motion, UTheo  = 73588 ± 2298 yr, and found to be in good agreement within errors, hence verifying general relativity theory once again.

scholarly journals Identification of binary and multiple systems in TGAS using the Virtual Observatory

2017 ◽  
Vol 12 (S330) ◽  
pp. 225-226
Author(s):  
F. Jiménez-Esteban ◽  
E. Solano
Keyword(s):  
Binary Systems ◽  
Virtual Observatory ◽  
Multiple Star ◽  
Multiple Systems ◽  
Multiple Stars ◽  
Stellar Formation ◽  
Virtual Observatory Tools ◽  
Formation And Evolution ◽  
Collapsing Cloud ◽  
Cloud Core

AbstractBinary and multiple stars have long provided an effective method of testing stellar formation and evolution theories. In particular, wide binary systems with separations > 20,000 au are particularly challenging as their physical separations are beyond the typical size of a collapsing cloud core (5,000 - 10,000 au). We present here a preliminary work in which we make use of the TGAS catalogue and Virtual Observatory tools and services (Aladin, TOPCAT, STILTS, VOSA, VizieR) to identify binary and multiple star candidate systems. The catalogue will be available from the Spanish VO portal (http://svo.cab.inta-csic.es) in the coming months.

scholarly journals X-ray and UV emission of the ultrashort-period, low-mass eclipsing binary system BX Trianguli

2018 ◽  
Vol 619 ◽  
pp. A138
Author(s):  
V. Perdelwitz ◽  
S. Czesla ◽  
J. Robrade ◽  
T. Pribulla ◽  
J. H. M. M. Schmitt
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Binary Systems ◽  
Uv Light ◽  
Close Binary ◽  
Eclipsing Binary ◽  
X Ray ◽  
Uv Emission ◽  
Low Mass ◽  
Orbital Modulation

Context.Close binary systems provide an excellent tool for determining stellar parameters such as radii and masses with a high degree of precision. Due to the high rotational velocities, most of these systems exhibit strong signs of magnetic activity, postulated to be the underlying reason for radius inflation in many of the components. Aims.We extend the sample of low-mass binary systems with well-known X-ray properties. Methods.We analyze data from a singular XMM-Newton pointing of the close, low-mass eclipsing binary system BX Tri. The UV light curve was modeled with the eclipsing binary modeling tool PHOEBE and data acquired with the EPIC cameras was analyzed to search for hints of orbital modulation. Results.We find clear evidence of orbital modulation in the UV light curve and show that PHOEBE is fully capable of modeling data within this wavelength range. Comparison to a theoretical flux prediction based on PHOENIX models shows that the majority of UV emission is of photospheric origin. While the X-ray light curve does exhibit strong variations, the signal-to-noise ratio of the observation is insufficient for a clear detection of signs of orbital modulation. There is evidence of a Neupert-like correlation between UV and X-ray data.

Phase transition-induced changes in the Raman properties of DMSO/benzene binary systems

2021 ◽  
Vol 23 (15) ◽  
pp. 9211-9217
Author(s):  
Guannan Qu ◽  
Rasheed Bilal ◽  
Minsi Xin ◽  
Zhong Lv ◽  
Guangyong Jin ◽  
...  
Keyword(s):  
Phase Transition ◽  
Hydrogen Bond ◽  
Binary System ◽  
Binary Systems ◽  
Induced Changes

Hydrogen bond generated between DMSO and benzene binary system induced changes in the Raman properties during phase transition.

scholarly journals A New Revision of the HDEC (Henry Draper Extension Charts) Catalog

2016 ◽  
Vol 25 (1) ◽  
Author(s):  
N. Ashimbaeva ◽  
V. Sementsov
Keyword(s):  
Binary Systems ◽  
Measurement Model ◽  
Spectral Classification ◽  
Multiple Systems ◽  
Cross Matching

AbstractA new version of the HDEC (Henry Draper Extension Charts) catalog is presented. The catalog includes 88,548 entries, more than 3500 of which (components of binary systems) were earlier corrupted by an algorithmic error (1579 multiple systems were revealed). Spectral classification of these objects has been corrected manually using the CDS data. We also corrected some mistakes of the catalog detected by the measurement model and cross-matching with other CDS catalogs, and, in some cases, by the authors of the catalog and through collaboration of the HDEC users.

scholarly journals The Hipparcos Double and Multiple Star Solutions

1998 ◽  
Vol 11 (1) ◽  
pp. 539-541
Author(s):  
F. Mignard
Keyword(s):  
Detailed Data ◽  
Multiple Star ◽  
Multiple Systems ◽  
Multiple Stars ◽  
Different Types ◽  
Hipparcos Catalogue ◽  
Double And Multiple Stars

Abstract The Hipparcos Catalogue provides general astrometric and photometric information on double and multiple stars in specific fields of the main Catalogue and detailed data on the components in the various sections of a dedicated annex: the Double and Multiple Systems Annex (DMSA). Overall statistics of these solutions are presented for the 13211 entries of this annex and the different types of solutions are outlined.

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