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Alfvén waves in low mass star forming regions

Alfvén waves in low mass star forming regions

... of Alfvén wave support considered in the remaining chapters involve the contribu tio n of any heating by the waves to the the rmal equilibrium, and the stability of the model ...a low-mass sta ... See full document

178

Testing the universality of star formation - I. Multiplicity in nearby star-forming regions

Testing the universality of star formation - I. Multiplicity in nearby star-forming regions

... primary mass (Duquennoy & Mayor 1991; Fischer & Marcy 1992; Lada ...primary mass (at least from M dwarfs to G dwarfs), and so this mass dependence may reflect a primordial ... See full document

18

Punanova, Anna
  

(2017):


	Chemistry and kinematics in low-mass star-forming regions.


Dissertation, LMU München: Fakultät für Physik

Punanova, Anna (2017): Chemistry and kinematics in low-mass star-forming regions. Dissertation, LMU München: Fakultät für Physik

... This work has found a large range of deuterium fractions across L1688, from a minimum of 2% to a maximum of 43%. Previous studies of deuterium fraction did not show such a big spread: for example, 525% in Taurus (Crapsi ... See full document

167

The physical and chemical evolution of star forming regions

The physical and chemical evolution of star forming regions

... outer regions of a m olecular cloud is generally at least 10"4 because th e gas phase carbon rem ains prim arily in C"*" due to th e efficiency of photodissociation and photoionization processes, ... See full document

147

Methods and Results Toward Measuring Magnetic Fields in Star-Forming Regions

Methods and Results Toward Measuring Magnetic Fields in Star-Forming Regions

... of star formation and evolution, and the cycle of insterstellar material, including dust grains and ...the star formation process (Mouschovias 2001), especially in the low-mass ... See full document

142

Ultracool dwarfs in open clusters and star-forming regions

Ultracool dwarfs in open clusters and star-forming regions

... and mass functions using the NextGen and DUSTY models from the Lyon group for consistency [31, ...to low-mass stars and brown dwarfs. The mass functions for Per, the Pleiades, and Praesepe are ... See full document

7

Disk Outflow Models as Applied to High Mass Star Forming Regions through Methanol and Water Maser Observations

Disk Outflow Models as Applied to High Mass Star Forming Regions through Methanol and Water Maser Observations

... high mass star formation is a scaled-up version of the low mass star formation process, complete with disk and outflows, or whether high mass stars form by coalescence of ... See full document

28

The evolution of post starburst galaxies from z=2 to 0 5

The evolution of post starburst galaxies from z=2 to 0 5

... different regions of super-colour ...recent star formation (quiescent galaxies) form a tight and well-defined ‘red sequence’ with low ...The star-forming population of galaxies covers a ... See full document

13

Comparisons between different techniques for measuring mass segregation

Comparisons between different techniques for measuring mass segregation

... observed star-forming regions display a range of fractal dimensions (Cartwright & Whitworth 2004; Schmeja et ...all regions may form with the same (low) fractal dimension, and ob- ... See full document

14

Weak and compact radio emission in early high mass star forming regions  II  The nature of the radio sources

Weak and compact radio emission in early high mass star forming regions II The nature of the radio sources

... In Rosero et al. ( 2016, hereafter Paper I ) we described our high-sensitivity (∼ 3 – 10 μ Jy beam − 1 ) continuum survey, which aimed to identify candidates in early evolutionary phases of high-mass star ... See full document

23

Fragmentation and disk formation during high-mass star formation. IRAM NOEMA (Northern Extended Millimeter Array) large program CORE

Fragmentation and disk formation during high-mass star formation. IRAM NOEMA (Northern Extended Millimeter Array) large program CORE

... lower mass fragments close to the global Jeans mass were not detected in these ...lower mass fragments (Zhang et ...less-evolved regions such as those in Wang et ...of low-mass ... See full document

28

Testing the universality of star formation - II. Comparing separation distributions of nearby star-forming regions and the field

Testing the universality of star formation - II. Comparing separation distributions of nearby star-forming regions and the field

... et al. 1999). Due to the dispersion of this cluster, searches for mem- bers are incomplete, but > 100 high-mass members have been iden- tified through their proper motion and parallaxes (de Zeeuw et al. 1999) ... See full document

11

Spitzer IRAC Colors of Nebulae Associated with Star Forming Regions

Spitzer IRAC Colors of Nebulae Associated with Star Forming Regions

... II regions, W5-East (W5-E) and W5-West. The ionizing star in W5-E is an O7V star, BD +59˚ ...of low-mass stars in this ...small regions to investigate the nebular color (Figure ... See full document

12

1-10 Myr-old Low Mass Stars and Brown Dwarfs in Nearby Star Forming Regions

1-10 Myr-old Low Mass Stars and Brown Dwarfs in Nearby Star Forming Regions

... higher mass stellar members of USco with spectral types B–M5 ...the low mass brown ...a mass range from ∼ ...shape low mass ... See full document

222

Water in low-mass star-forming regions with Herschel

Water in low-mass star-forming regions with Herschel

... and low gas-phase wa- ter abundances in cold clouds appears well established, there are only a few sources for which both ice and gas have been ob- served along the same line of ...warm regions was ... See full document

19

1-10 Myr-old low mass stars and brown dwarfs in nearby star forming regions

1-10 Myr-old low mass stars and brown dwarfs in nearby star forming regions

... intermediate mass stellar IMF is greatly overshadowed by our relative non-existent understand- ing of the lowest mass stellar and substellar end of the mass ...high mass end of the IMF. ... See full document

12

Looking deep into the Rosette Nebula's heart : the (sub)stellar content of the massive young cluster NGC 2244

Looking deep into the Rosette Nebula's heart : the (sub)stellar content of the massive young cluster NGC 2244

... between low-mass stars and BDs is typically found in the range 2 – ...the star-to-BD ratio ( uncertainties in distances, ages, use of different evolutionary models, reddening laws, membership issues, ... See full document

22

The JCMT Gould Belt Survey : low mass protoplanetary discs from a SCUBA 2 census of NGC 1333

The JCMT Gould Belt Survey : low mass protoplanetary discs from a SCUBA 2 census of NGC 1333

... environment. Star formation regions vary greatly, from spare associations such as in Taurus– Auriga up to dense clusters exemplified by the Orion nebula ...entire regions and for systematically ... See full document

6

Apparent cross field superslow propagation of magnetohydrodynamic waves in solar plasmas

Apparent cross field superslow propagation of magnetohydrodynamic waves in solar plasmas

... continuum Alfvén waves and / or continuum slow waves in the magnetic structures of the solar atmosphere as, ...continuum waves is apparent because there is no real propagation of energy across ... See full document

12

On the reflection of Alfvén waves in an ideal magnetoatmosphere

On the reflection of Alfvén waves in an ideal magnetoatmosphere

... As a result, the magnetic field produces a nonabsorbing critical layer, below it the solution can be written as a linear combination of an upward and a downward propagating wave with the[r] ... See full document

6

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