Possible biotic distribution in our galaxy

Peña-Cabrera, G. V. Y.; Durand-Manterola, H. J.

doi:10.1016/j.asr.2003.07.016

Cited by 19 publications

(15 citation statements)

References 5 publications

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“…This complies with the results on Galactic habitable zone in Peña-Cabrera & Durand-Manterola (2004), where the zone of enhanced habitability probability is estimated to be at ρ = (4, 17.5) kpc. Our results differ from ρ = (7, 9) kpc conservative estimates in Lineweaver, Fenner & Gibson (2004) probably caused by calibrating threshold habitability values of SFR and stellar density to Solar neighbourhood.…”

Section: Wider Ghz?supporting

confidence: 76%

“…At first look it seems that higher metallicity of interstellar matter will yield higher number of rocky planets, but this need not be the case. The "goldilocks" approach taken by Lineweaver (2001);Peña-Cabrera & Durand-Manterola (2004) relies on the assumption that high metallicity is likely to lead to formation of gas giants with rocky cores, preferentially via core accretion model (see also, Buchhave et al, 2012;Ikoma, Nakazawa & Emori, 2000). The samples of exoplanets show that the highest number of discovered systems have hosts with near Solar metallicity.…”

Section: Habitability Agentsmentioning

confidence: 99%

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‘Grandeur in this view of life’:N-body simulation models of the Galactic habitable zone

Vukotić

Steinhauser

Martinez-Aviles

et al. 2016

Mon. Not. R. Astron. Soc.

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We present an isolated Milky Way-like simulation in GADGET2 Nbody SPH code. The Galactic disk star formation rate (SFR) surface densities and stellar mass indicative of Solar neighbourhood are used as thresholds to model the distribution of stellar mass in life friendly environments. SFR and stellar component density are calculated averaging the GADGET2 particle properties on a 2D grid mapped on the Galactic plane. The peak values for possibly habitable stellar mass surface density move from 10 to 15 kpc cylindrical galactocentric distance in 10 Gyr simulated time span. At 10 Gyr the simulation results imply the following. Stellar particles which have spent almost all of their life time in habitable friendly conditions reside typically at ∼ 16 kpc from Galactic centre and are ∼ 3 Gyr old. Stellar particles that have spent ≥ 90% of their 4 − 5 Gyr long life time in habitable friendly conditions, are also predominantly found in the outskirts of the Galactic disk. Less then 1% of these particles can be found at a typical Solar system galactocentric distance of 8 − 10 kpc. Our results imply that the evolution of an isolated spiral galaxy is likely to result in galactic civilizations emerging at the outskirts of the galactic disk around stellar hosts younger than the Sun.

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Section: Wider Ghz?supporting

confidence: 76%

Section: Habitability Agentsmentioning

confidence: 99%

‘Grandeur in this view of life’:N-body simulation models of the Galactic habitable zone

Vukotić

Steinhauser

Martinez-Aviles

et al. 2016

Mon. Not. R. Astron. Soc.

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“…(Although, of course, the exact value depends on still poorly understood effects of close supernovae on planetary environments.) The same general conclusion follows from the estimate of Pena-Cabrera and Durand-Manterola (2004), who find R inn = 4 kpc, on the basis of the assumption that metal-rich planets in the inner Galaxy would grow too fast to be inhabitable; this assumption, however, is highly questionable since another kind of habitable planets could plausibly form under high-Z conditions (see, e.g. Léger et al 2004).…”

Section: Inner Boundarysupporting

confidence: 56%

“…The first two has been proposed in a qualitative manner by Gonzalez et al (2001), and subsequently quantified by Lineweaver et al (2004). The third has been proposed by Pena-Cabrera and Durand-Manterola (2004); they have considered only suppression of terrestrial planets Boundaries of the habitable zone 115 due to very high Z. Photoevaporation of protoplanetary disks have been considered in a different context by Adams et al (2004); its application to GHZ remains to be done.…”

Section: Inner Boundarymentioning

confidence: 99%

Boundaries of the habitable zone: unifying dynamics, astrophysics, and astrobiology

Ćirković

2004

Proc. IAU

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Abstract. We are witnessing tremendous progress in the nascent multidisciplinary field of astrobiology, encompassing the origin and evolution of life in the cosmic context. One of the key concepts recently introduced in this field is the Galactic Habitable Zone (GHZ): an interval of galactocentric distances convenient for formation of stars possessing habitable planets. The boundaries of the GHZ are still poorly understood, however. Here we present a comparative analysis of various proposals for the mechanisms determining the GHZ boundaries, as well as different numerical values obtained. When joined with the models of Galactic stellar distribution, this gives us a better handle on the number of potential life-bearing sites.

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“…Rasool&DeBergh 1970, Hart 1979,1978, Kasting et al 1993, Selsis et al 2007, Williams&Pollard 2002, Peña--Cabrera & Durand--Manterola 2004, Buccino et al 2006, VonBloh et al 2007, Spiegel et al 2009). The main differences are in the climatic constraints imposed on the limits of the HZ by these studies.…”

Section: Introductionmentioning

confidence: 99%

EXPLORING THE HABITABLE ZONE FOR KEPLER PLANETARY CANDIDATES

Kaltenegger

Sasselov

2011

ApJ

103

118

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This paper outlines a simple approach to evaluate habitability of terrestrial planets by assuming different types of planetary atmospheres and using corresponding model calculations. Our approach can be applied for current and future candidates provided by the Kepler mission and other searches. The resulting uncertainties and changes in the number of planetary candidates in the HZ for the Kepler February 2011 data release are discussed. To first order the HZ depends on the effective stellar flux distribution in wavelength and time, the planet albedo, and greenhouse gas effects. We provide a simple set of parameters which can be used for evaluating current and future planet candidates from transit searches. Subject headings: Astrobiology --atmospheric effects --methods: data analysisEarth --planets and satellites: general -stars: individual (Kepler) IntroductionThe NASA Kepler mission recently announced 1235 planetary candidates (Borucki et al. 2011). We use atmospheric models to explore the potential for habitability of Kepler planetary candidates.The habitable zone (HZ) concept was proposed for the first time by Huang (1959Huang ( , 1960 and has been calculated by several authors after that (see e.g. Rasool&DeBergh 1970, Hart 1979,1978, Kasting et al. 1993, Selsis et al. 2007, Williams&Pollard 2002, Peña--Cabrera & Durand--Manterola 2004, Buccino et al. 2006, VonBloh et al. 2007, Spiegel et al. 2009). The main differences are in the climatic constraints imposed on the limits of the HZ by these studies. We focus on the circumstellar HZ, that was defined by Kasting et al. (1993) as an annulus around a star where a planet with an atmosphere and a sufficiently large water content like Earth can host liquid water permanently on a solid surface. This definition of the HZ implies surface habitability because it is defined to allow remote detectability of life as we know it. Kepler planetary candidates with radii below 2 Earth's radii are consistent with models of potentially rocky planets.The two edges of the HZ are influenced by the relationship between the albedo of the planet and the effective temperature of the star (Fig.1). In this definition the inner edge of the HZ is defined as the location where the entire water reservoir can be vaporized by runaway greenhouse conditions, followed by the photo-dissociation of water vapor and subsequent escape of free hydrogen into space. The outer boundary is defined as the distance from the star where the maximum greenhouse effect fails to keep CO 2 from condensing Kaltenegger & Sasselov 2011 accepted ApJL 2 permanently, leading to runaway glaciation. Subsurface life that could exist on planets or moons with very different surface temperatures is not considered, because of the lack of atmospheric features that could be used to remotely assert habitability on such an object (Rosing 2005). We will not discuss the issue of life emerging in other solvents here.Note that a planet found in the HZ is not necessarily habitable, since many factors may prevent habitabili...

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Possible biotic distribution in our galaxy

Cited by 19 publications

References 5 publications

‘Grandeur in this view of life’:N-body simulation models of the Galactic habitable zone

‘Grandeur in this view of life’:N-body simulation models of the Galactic habitable zone

Boundaries of the habitable zone: unifying dynamics, astrophysics, and astrobiology

EXPLORING THE HABITABLE ZONE FOR KEPLER PLANETARY CANDIDATES

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