scholarly journals Design Considerations for a Ground-Based Transit Search for Habitable Planets Orbiting M Dwarfs

2008 ◽  
Vol 120 (865) ◽  
pp. 317-327 ◽  
Author(s):  
Philip Nutzman ◽  
David Charbonneau
Keyword(s):  
M Dwarfs ◽  
Habitable Planets ◽  
Design Considerations

On the Growth and Detectability of Land Plants on Habitable Planets around M Dwarfs

Astrobiology ◽  
2017 ◽  
Vol 17 (12) ◽  
pp. 1219-1232 ◽  
Author(s):  
Duo Cui ◽  
Feng Tian ◽  
Yuwei Wang ◽  
Changshen Li ◽  
Chaoqing Yu ◽  
...  
Keyword(s):  
Land Plants ◽  
M Dwarfs ◽  
Habitable Planets

scholarly journals THE IMPACT OF STELLAR ROTATION ON THE DETECTABILITY OF HABITABLE PLANETS AROUND M DWARFS

2016 ◽  
Vol 821 (1) ◽  
pp. L19 ◽  
Author(s):  
Elisabeth R. Newton ◽  
Jonathan Irwin ◽  
David Charbonneau ◽  
Zachory K. Berta-Thompson ◽  
Jason A. Dittmann
Keyword(s):  
Stellar Rotation ◽  
M Dwarfs ◽  
Habitable Planets ◽  
The Impact

scholarly journals Why do we find ourselves around a yellow star instead of a red star?

2017 ◽  
Vol 17 (1) ◽  
pp. 77-86 ◽  
Author(s):  
Jacob Haqq-Misra ◽  
Ravi Kumar Kopparapu ◽  
Eric T. Wolf
Keyword(s):  
Bayesian Inference ◽  
Habitable Zone ◽  
M Dwarfs ◽  
Dwarf Stars ◽  
Habitable Planets ◽  
Chance Event ◽  
The Future ◽  
M Dwarf Stars ◽  
M Dwarf

AbstractM-dwarf stars are more abundant than G-dwarf stars, so our position as observers on a planet orbiting a G-dwarf raises questions about the suitability of other stellar types for supporting life. If we consider ourselves as typical, in the anthropic sense that our environment is probably a typical one for conscious observers, then we are led to the conclusion that planets orbiting in the habitable zone of G-dwarf stars should be the best place for conscious life to develop. But such a conclusion neglects the possibility that K-dwarfs or M-dwarfs could provide more numerous sites for life to develop, both now and in the future. In this paper we analyse this problem through Bayesian inference to demonstrate that our occurrence around a G-dwarf might be a slight statistical anomaly, but only the sort of chance event that we expect to occur regularly. Even if M-dwarfs provide more numerous habitable planets today and in the future, we still expect mid G- to early K-dwarfs stars to be the most likely place for observers like ourselves. This suggests that observers with similar cognitive capabilities as us are most likely to be found at the present time and place, rather than in the future or around much smaller stars.

scholarly journals In situ models for planet assembly around cool stars

2014 ◽  
Vol 14 (2) ◽  
pp. 267-278 ◽  
Author(s):  
Brad M. S. Hansen
Keyword(s):  
Water Content ◽  
Planetary System ◽  
Habitable Zone ◽  
Water Delivery ◽  
M Dwarfs ◽  
Transit Systems ◽  
Produce Water ◽  
Habitable Planets ◽  
Cool Stars

AbstractWe present a model for the in situ assembly of planetary systems around a 0.5 M⊙ star, and compare the resulting statistics with the observed sample of cool Kepler planet candidates. We are able to reproduce the distribution of planetary periods and period ratios, although we once again find an underabundance of single transit systems relative to the observations. We also demonstrate that almost every planetary system assembled in this fashion contains at least one planet in the habitable zone, and that water delivery to these planets can potentially produce water content comparable to that of Earth. Our results broadly support the notion that habitable planets are plentiful around M dwarfs in the solar neighbourhood.

Titan and habitable planets around M-dwarfs

2010 ◽  
Vol 147 ◽  
pp. 405 ◽  
Author(s):  
Jonathan I. Lunine
Keyword(s):  
M Dwarfs ◽  
Habitable Planets

Morphological behavior of compatibilized ternary blends prepared by mechanical mixing

1993 ◽  
Vol 51 ◽  
pp. 1200-1201
Author(s):  
S.D. Smith ◽  
R.J. Spontak ◽  
D.H. Melik ◽  
S.M. Buehler ◽  
K.M. Kerr ◽  
...  
Keyword(s):  
Interfacial Adhesion ◽  
Diblock Copolymers ◽  
Ternary Blends ◽  
Mechanical Mixing ◽  
Design Considerations ◽  
Covalently Bonded ◽  
Homopolymer Blends ◽  
Emulsifying Agent ◽  
Surface Active ◽  
Low Entropy

When blended together, homopolymers A and B will normally macrophase-separate into relatively large (≫1 μm) A-rich and B-rich phases, between which exists poor interfacial adhesion, due to a low entropy of mixing. The size scale of phase separation in such a blend can be reduced, and the extent of interfacial A-B contact and entanglement enhanced, via addition of an emulsifying agent such as an AB diblock copolymer. Diblock copolymers consist of a long sequence of A monomers covalently bonded to a long sequence of B monomers. These materials are surface-active and decrease interfacial tension between immiscible phases much in the same way as do small-molecule surfactants. Previous studies have clearly demonstrated the utility of block copolymers in compatibilizing homopolymer blends and enhancing blend properties such as fracture toughness. It is now recognized that optimization of emulsified ternary blends relies upon design considerations such as sufficient block penetration into a macrophase (to avoid block slip) and prevention of a copolymer multilayer at the A-B interface (to avoid intralayer failure).

Theoretical And Practical Design Considerations for Ultra-High Resolution Electron Lenses

1980 ◽  
Vol 38 ◽  
pp. 266-269
Author(s):  
Y. Harada ◽  
K. Tsuno ◽  
Y. Arai
Keyword(s):  
Optical Properties ◽  
High Resolution ◽  
Chromatic Aberration ◽  
Point Of View ◽  
Pole Piece ◽  
Axial Field ◽  
Design Considerations ◽  
Resolution Electron ◽  
Practical Design ◽  
Peak Flux

Magnetic objective lenses, from the point of view of pole piece geometry, can he roughly classified into two types, viz., symmetrical and asymmetrical. In the case of the former, the optical properties have been calculated by several authors1-3) and the results would appear to suggest that, in order to reduce the spherical and chromatic aberration coefficients, Cs and Cc, it is necessary to decrease the half-width value of the axial field distribution and to increase the peak flux density. The expressions for either minimum Cs or minimum Cc were presented in the form of ‘universal’ curves by Mulvey and Wallington4).

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