Principles of Star Formation

Bodenheimer, Peter

doi:10.1007/978-3-642-15063-0

Cited by 70 publications

(52 citation statements)

References 366 publications

(563 reference statements)

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“…Using our sample and the literature, we calculate: f(∆ m ≥0.7 mag) ∼28%, f(∆ m ≥0.6 mag) ∼42%, and f(∆ m ≥0.5 mag) ∼40%. Theses estimates do not include 1995 QY 9 and Arawn as we assume they are elongated objects.…”

Section: Fraction Of Contact Binaries In the Plutino Populationmentioning

confidence: 99%

“…Even if it is still unclear how contact binaries are formed, one can argue that tidal effects as suggested by Porter & Grundy (2012) can create very tight orbits, but the gravitational collapse is also an option (Nesvorný et al 2010). Finally, as suggested by the star formation theory, if a triple system looses one component, the other two objects have to shrink their orbit to go back to a stable configuration and can potentially create a contact/close binary (Bodenheimer 2011). However, it is important to point out that several of theses models are not dedicated to the TNO science, and that we are still missing several observables to infer if a model is working or not.…”

Section: Introductionmentioning

confidence: 99%

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The Plutino Population: An Abundance of Contact Binaries

Thirouin

Sheppard²

2018

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We observed twelve Plutinos over two separated years with the 4.3m Lowell's Discovery Channel Telescope. Here, we present the first lightcurve data for those objects. Three of them (2014 JL 80 , 2014 JO 80 , 2014 JQ 80 ) display a large lightcurve amplitude explainable by a single elongated object, but are most likely caused by a contact binary system due to their lightcurves morphology. These potential contact binaries have rotational periods from 6.3 h to 34.9 h and peak-to-peak lightcurve variability between 0.6 and 0.8 mag. We present partial lightcurves allowing us to constrain the lightcurve amplitude and the rotational period of another nine Plutinos. By merging our data with the literature, we estimate that up to ∼40% of the Plutinos could be contact binaries. Interestingly, we found that all the suspected contact binaries in the 3:2 resonance are small with absolute magnitude H>6 mag. Based on our sample and the literature, up to ∼50% of the small Plutinos are potential contact binaries.

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Section: Fraction Of Contact Binaries In the Plutino Populationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Plutino Population: An Abundance of Contact Binaries

Thirouin

Sheppard²

2018

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“…The typical masses of core are about 1 to a few M ⊙ , although a few range up to 1000 M ⊙ . The clumps are surrounded by a low density envelope which have a typical dimension of ≈ 10 4 − 10 6 AU (Bodenheimer 2011). Magnetic fields play a significant role in collapse dynamics by mediating accretion, directing the outflows and collimating jets (Li & Nakamura 2004;Galli 2009).…”

Section: Introductionmentioning

confidence: 99%

Magnetic field geometry of the large globule CB 34

Das

Medhi

et al. 2016

Astrophys Space Sci

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We report the results of optical polarimetric observations of a Bok globule CB34 to study magnetic field structure on large scales (10 5 − 10 6 AU), which is combined with archival sub-mm observations to characterize the magnetic field structure of CB34 on small scales (10 4 −10 5 AU). The optical polarization measurements indicate that the magnetic field in the globule is constrained to a maximum radius of 10 5 AU around the core, out to densities not smaller than 10 4 cm −3 . Our study is mainly concentrated on two submillimeter cores C1 and C2 of CB34. The direction of magnetic field of core C2 is found to be nearly perpendicular to the CO outflow direction of the globule. The magnetic field of core C1 is almost aligned with the minor axis of the core which is typical for magnetically dominated star formation models. The mean value of offset between the minor axis of core C2 and the outflow direction is found to be 14• which suggests that the direction of the outflow is almost aligned with the minor axis of core C2. The magnetic field strength in the plane-ofsky for cores C1 and C2 is estimated to be ≈ 34µG and ≈ 70µG.

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“…The density tested from all 14 models have ranges between 0.003 ∼ 50 solar mass per pc 3 , the corresponding hydrogen number density is 0.004 ∼ 70 cm −3 . To put this into observational perspectives, the giant molecular clouds have density n(H 2 )(cm −3 ) of 100, molecular clouds have the density of 300, molecular clumps have the density around 10 3 , and cloud cores have density 10 5 (Bodenheimer 2011). Thus the tested simulation cubes can be applied to giant molecular clouds which have similar number densities.…”

Section: Effects Of Self-gravitymentioning

confidence: 99%

Tracing Magnetic Field Morphology Using the Velocity Gradient Technique in the Presence of CO Self-absorption

Hsieh

Lai

et al. 2019

ApJ

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Probing magnetic fields in self-gravitating molecular clouds are generally difficult even with the use of the polarimetry. Based on the properties of magneto-hydrodynamic (MHD) turbulence and turbulent reconnection, Velocity Gradient Technique (VGT) provides a new way in tracing magnetic field orientation and strength based on the spectroscopic data. Our study tests the applicability of VGT in various molecular tracers, e.g. 12 CO, 13 CO, and C 18 O. By inspecting synthetic molecular line maps of CO isotopologue generated through radiative transfer calculations, we show that the VGT method can be successfully applied in probing the magnetic field direction in the diffuse interstellar medium as well as in self-gravitating molecular clouds.

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Principles of Star Formation

Cited by 70 publications

References 366 publications

The Plutino Population: An Abundance of Contact Binaries

The Plutino Population: An Abundance of Contact Binaries

Magnetic field geometry of the large globule CB 34

Tracing Magnetic Field Morphology Using the Velocity Gradient Technique in the Presence of CO Self-absorption

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