A Giant Planet Imaged in the Disk of the Young Star β Pictoris

By Anne-Marie Lagrange, M. Bonnefoy, G. Chauvin, D. Apai, David Ehrenreich, Anthony Boccaletti, D. Gratadour, D. Rouan, David Mouillet, S. Lacour and 1 more. Science, 2010

716 citations recorded by the source corpus.

Planet Is Born The 10-million-year-old star β Pictoris, has long been suspected to host a planet. Through images obtained with the Very Large Telescope, an array of four telescopes located in Chile, Lagrange et al. (p. 57, published online 10 June) now confirm the presence of a young, giant planet, β Pictoris b, orbiting within the dusty disk that surrounds the star. β Pictoris b orbits closer to its star than Uranus and Neptune do to the Sun in our solar system. This orbital separation is consistent with the in situ formation of the planet via a core accretion mechanism. Thus, giant planets can form within a stellar dust disk in only a few million years. The Very Large Telescope reveals that a huge planet formed within a star’s dusty disk in a few million years. Here, we show that the ~10-million-year-old β Pictoris system hosts a massive giant planet, β Pictoris b, located 8 to 15 astronomical units from the star. This result confirms that gas giant planets form rapidly within disks and validates the use of disk structures as fingerprints of embedded planets. Among the few planets already imaged, β Pictoris b is the closest to its parent star. Its short period could allow for recording of the full orbit within 17 years.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

• First light of the VLT planet finder SPHERE - III. New spectrophotometry and astrometry of the HR 8799 exoplanetary system (2015, background): “…wide (>5 au) separations (e.g., Chauvin et al. 2005a,b; Itoh et al. 2005; Luhman et al. 2006, 2007; Marois et al. 2008, 2010b; Thalmann et al. 2009; Lagrange et al. 2010; Biller et al. 2010; Mugrauer et al. 2010; Lafrenière et al. 2010; Carson et al. 2013; Kuzuhara et al. 2013; Rameau et al.…”
• A lithium depletion boundary age of 21 Myr for the Beta Pictoris moving group (2013, background): “Studies that exploit the youth and proximity of BPMG members include: the identification and direct imagingof a planet (e.g. Lagrange et al. 2010, 2012; Bonnefoy et al. 2011, 2013) and debris disc (e.g. Smith & Terrile 1984; Holland et al. 1998; Golimowski et al. 2006) around its most luminous…”
• A New High Contrast Imaging Program at Palomar Observatory (2010, background): “Moreover, recent results (Marois et al. 2008; Kalas et al. 2008; Lagrange et al. 2010) have demonstrated that direct imaging of planetary mass companions and disks (Oppenheimer et al. 2008; Hinkley et al. 2009; Mawet et al. 2009; Boccaletti et al. 2009) is a technique 1 Department of Astronomy,…”
• Stellar and substellar companions of nearby stars from Gaia DR2 (2018, background): “The GDR2 record of β Pic lists a high value of the astrometric excess noise i = 2.14 mas (Table 1), that indicates that the astrometric fit shows the presence of significant residuals.”
• A COMBINED SUBARU/VLT/MMT 1–5 μm STUDY OF PLANETS ORBITING HR 8799: IMPLICATIONS FOR ATMOSPHERIC PROPERTIES, MASSES, AND FORMATION (2011, background): “Along with Fomalhaut and β Pic, it is also the only imaged system with companion mass ratios and separations reasonably close to the giant planets in the Solar System (Kalas et al. 2008; Lagrange et al. 2009, 2010)10.”
• Adaptive Optics for Astronomy (2012, background): “This has been suggested for the ∼ 9MJ planet β Pic b, also discovered by AO imaging, which orbits a 1.8M⊙ star at a distance of 8–15AU (Lagrange et al. 2010) (Fig.”
• DETECTION AND CHARACTERIZATION OF EXOPLANETS AND DISKS USING PROJECTIONS ON KARHUNEN–LOÈVE EIGENIMAGES (2012, background): “…structures orbiting nearby stars were 1Space Telescope Science Institute, 3700 San Martin Drive, Baltimore MD 21218, USA obtained relatively recently (Marois et al. 2008a; Kalas et al. 2008; Lagrange et al. 2009, 2010; Marois et al. 2010b; Kalas 2011; Janson et al. 2012; Kraus & Ireland 2012).”
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• ORBITAL MOTION OF HR 8799 b, c, d USING HUBBLE SPACE TELESCOPE DATA FROM 1998: CONSTRAINTS ON INCLINATION, ECCENTRICITY, AND STABILITY (2011, background): “The first images of planets orbiting nearby stars have been obtained relatively recently (Marois et al. 2008; Kalas et al. 2008; Lagrange et al. 2009, 2010; Marois et al. 2010b) and followed up at different wavelengths (Quanz et al. 2010; Currie et al. 2011b; Bonnefoy et al. 2011).”
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• THE GEMINI/NICI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF PLANETS AROUND YOUNG MOVING GROUP STARS (2013, background): “…known to date, most have been discovered around A stars (HR 8799bcde, Fomalhaut b, β Pic b, WD 0806-661; Marois et al. 2008, 2010; Kalas et al. 2008; Lagrange et al. 2009, 2010; Luhman et al. 2011; Quanz et al. 2013; Rameau et al. 2013b), with a few also discovered around very young solar analogs…”
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