THE HABITABLE ZONES OF PRE-MAIN-SEQUENCE STARS

@article{Ramirez2014THEHZ,
  title={THE HABITABLE ZONES OF PRE-MAIN-SEQUENCE STARS},
  author={Ramses Mario Ramirez and Lisa Kaltenegger},
  journal={The Astrophysical Journal Letters},
  year={2014},
  volume={797}
}
We calculate the pre-main-sequence habitable zone (HZ) for stars of spectral classes F–M. The spatial distribution of liquid water and its change during the pre-main-sequence phase of protoplanetary systems is important for understanding how planets become habitable. Such worlds are interesting targets for future missions because the coolest stars could provide habitable conditions for up to 2.5 billion years post-accretion. Moreover, for a given star type, planetary systems are more easily… 

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References

SHOWING 1-10 OF 47 REFERENCES

HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: NEW ESTIMATES

Identifying terrestrial planets in the habitable zones (HZs) of other stars is one of the primary goals of ongoing radial velocity (RV) and transit exoplanet surveys and proposed future space

HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: DEPENDENCE ON PLANETARY MASS

The ongoing discoveries of extra-solar planets are unveiling a wide range of terrestrial mass (size) planets around their host stars. In this Letter, we present estimates of habitable zones (HZs)

Habitable zones around main sequence stars.

The results suggest that mid-to-early K stars should be considered along with G stars as optimal candidates in the search for extraterrestrial life.

Stabilizing Cloud Feedback Dramatically Expands the Habitable Zone of Tidally Locked Planets

The habitable zone (HZ) is the circumstellar region where a planet can sustain surface liquid water. Searching for terrestrial planets in the HZ of nearby stars is the stated goal of ongoing and

A REVISED ESTIMATE OF THE OCCURRENCE RATE OF TERRESTRIAL PLANETS IN THE HABITABLE ZONES AROUND KEPLER M-DWARFS

Because of their large numbers, low-mass stars may be the most abundant planet hosts in our Galaxy. Furthermore, terrestrial planets in the habitable zones (HZs) around M-dwarfs can potentially be

A Decreased Probability of Habitable Planet Formation around Low-Mass Stars

Smaller terrestrial planets (≲0.3 M⊕) are less likely to retain the substantial atmospheres and ongoing tectonic activity probably required to support life. A key element in determining whether

EFFECT OF METALLICITY ON THE EVOLUTION OF THE HABITABLE ZONE FROM THE PRE-MAIN SEQUENCE TO THE ASYMPTOTIC GIANT BRANCH AND THE SEARCH FOR LIFE

During the course of stellar evolution, the location and width of the habitable zone changes as the luminosity and radius of the star evolves. The duration of habitability for a planet located at a

Remote life-detection criteria, habitable zone boundaries, and the frequency of Earth-like planets around M and late K stars

Climate-modeling calculations discussed here shed light on the width of the habitable zone around a star, and argue that conservative HZ definitions should be used for designing future space-based telescopes, but that optimistic definitions may be useful in interpreting the data from such missions.

Evolutionary models for low-mass stars and brown dwarfs: uncertainties and limits at very young ages

We analyse pre-Main Sequence evolutionary tracks for low mass stars with masses $m \\le 1.4 \\msol$ based on the Baraffe et al. (1998) input physics. We also extend the recent Chabrier et al. (2000)