[PDF] Top 20 The open flux evolution of a solar-mass star on the main sequence
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The open flux evolution of a solar-mass star on the main sequence
... active main- sequence solar-like ...momentum evolution models typically employ spin-down torques that are formulated in terms of the surface magnetic field ...the open flux, i.e. ... See full document
11
The open flux evolution of a solar mass star on the main sequence
... active main- sequence solar-like ...momentum evolution models typically employ spin-down torques that are formulated in terms of the surface magnetic field ...the open flux, i.e. ... See full document
11
Slingshot prominence evolution for a solar like star
... rotation evolution code to derive the properties of the formation and ejection of slingshot prominences during the lifetime of a star similar to our ...The mass, mass-loss rate, and rate of ... See full document
6
Coronal and heliospheric magnetic flux circulation and its relation to open solar flux evolution
... the solar cycle dependence of the HCS tilt [Owens and Lockwood, ...of sequence to the advancement of the solar cycle via their contribution to the polar field ... See full document
27
Variations in the slope of the resolved star-forming main sequence: a tool for constraining the mass of star-forming regions
... α MS Figure 3. The dependence of the rSFMS slope (α MS ) of the sim- ulated galaxies on pixel resolution. The colours and line styles indicate the slopes derived from different SFR tracers (instan- taneous, 10 Myr, 100 ... See full document
6
The main sequence of the star forming galaxies
... 1.2 The Star Formation Rate The star formation rate is the total mass of stars formed per year, often given as solar masses per year. The usual way to estimate such a rate is to derive it from ... See full document
31
The main sequence of star-forming galaxies - II. A non-evolving slope at the high-mass end
... However, once a larger part of the MS upper envelope is sampled by PACS data, as in the GOODS + CANDELS sam- ple, such artificial effect disappears (Fig. A4). Additionally, the MS location is evolving strongly as a ... See full document
17
Post Main Sequence Evolution Continued
... previous mass loss/outburst episodes. Material expelled from the star can have velocities in excess of 4000 to 10,000 ...net mass increase of the white dwarf in the binary system, it is possible that ... See full document
19
Post main sequence planetary system evolution
... the mass loss experienced in the post-MS evolution of the more massive star is adiabatic with respect to its daughter planetary system, but non-adiabatic with respect to the stellar binary ... See full document
66
Early stages of evolution and the main sequence phase
... the mass range 1.1 − 1.5 M ⊙ show a very similar behaviour after the main sequence, the only difference being the small convective core they develop during core ...the evolution track at ... See full document
52
Binary star influence on post main sequence multi planet stability
... during mass loss, after the star has become a white dwarf, then the system again becomes a fixed-mass system for which other theories may be ...our Solar Sytem but typically not in ... See full document
9
Reconciling the Observed Star-forming Sequence with the Observed Stellar Mass Function
... represent mass functions modulated by the mass-dependent destruction rates and growth rates from the Guo et ...the star-forming sequence required to make the evolution of the stellar ... See full document
16
An M Dwarf Companion to an F-type Star in a Young Main-sequence Binary
... primary star. The primary star is an early F-type main-sequence star with a mass of ( ...a mass of ( ...secondary star is among the lowest-mass M dwarfs ... See full document
7
Star/disk interaction and angular momentum evolution model for solar-like stars
... momentum evolution. It controls this latter one from the pre-main sequence, during the so-called disk locking phase where the stars magnetically interact with their surrounding disk, to the ... See full document
6
Low-mass stars: Open problems all along their evolution
... and evolution become increasingly evident, and can no longer be hidden under the carpet of observational ...pre-main sequence and continue throughout the complete ...the main sequence ... See full document
10
How is open solar magnetic flux lost over the solar cycle?
... coronal mass ejection (CME) rate. Assumptions of constant flux loss and loss proportional to the closed heliospheric flux are unable to reproduce two major features of the solar cycle ... See full document
13
The Evolution of Open Magnetic Flux Driven by Photospheric Dynamics
... physics. Two profoundly different views of the C0r0oa| magneticfield have emerged. In quasi-steady models, the predominantoource of open magneticfield iSiocoronal holes. In contrast, in [r] ... See full document
40
The lives of stars. Life on the Main Sequence. Stellar evolution : the lives of stars. Stellar Thermostat. Life on the Main Sequence.
... young star cluster contains many more massive blue stars on the Main Sequence than an old star ...the Main Sequence, the photospheres of stars cool down: they ‘evolve’ to the ... See full document
7
Spatially resolved star formation main sequence of galaxies in the CALIFA survey
... “main sequence of galaxies”—defined in terms of the total star formation rate ψ versus the total stellar mass M * —is a well-studied tight relation that has been observed at several wavelengths ... See full document
5
The SAMI Galaxy Survey : spatially resolving the main sequence of star formation
... the sequence with envi- ronmental ...the main sequence becomes more prominent at medium- and high- densities (log( 5 /Mpc − 2 ) > 0, > ...stellar mass surface density: the two-sided ... See full document
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