About

Robert Noyes is a Research Professor of Astronomy, Emeritus, at the Center for Astrophysics | Harvard & Smithsonian. His research interests include solar and stellar seismology, solar structure and dynamics, detection and characterization of planets around other stars, and the origin and evolution of planetary systems. His work involves studying the internal processes of the sun and stars through seismology, as well as exploring planetary systems beyond our own. Noyes's contributions are centered on understanding the fundamental mechanisms governing stellar behavior and planetary formation, utilizing observational data and theoretical models to advance knowledge in these areas.

Research topics

• Astrophysics
• Physics

Selected publications

• HAT-P-58b–HAT-P-64b: Seven Planets Transiting Bright Stars*

  The Astronomical Journal · 2021 · 11 citations

  • Physics
  • Astrophysics

  Abstract We report the discovery and characterization of seven transiting exoplanets from the HATNet survey. The planets, which are hot Jupiters and Saturns transiting bright Sun-like stars, include: HAT-P-58b (with mass M p = 0.37 M J , radius R p = 1.33 R J , and orbital period P = 4.0138 days), HAT-P-59b ( M p = 1.54 M J , R p = 1.12 R J , P = 4.1420 days), HAT-P-60b ( M p = 0.57 M J , R p = 1.63 R J , P = 4.7948 days), HAT-P-61b ( M p = 1.06 M J , R p = 0.90 R J , P = 1.9023 days), HAT-P-62b ( M p = 0.76 M J , R p = 1.07 R J , P = 2.6453 days), HAT-P-63b ( M p = 0.61 M J , R p = 1.12 R J , P = 3.3777 days), and HAT-P-64b ( M p = 0.58 M J , R p = 1.70 R J , P = 4.0072 days). The typical errors on these quantities are 0.06 M J , 0.03 R J , and 0.2 s, respectively. We also provide accurate stellar parameters for each of the host stars. With V = 9.710 ± 0.050 mag, HAT-P-60 is an especially bright transiting planet host, and an excellent target for additional follow-up observations. With R p = 1.703 ± 0.070 R J , HAT-P-64b is a highly inflated hot Jupiter around a star nearing the end of its main-sequence lifetime, and is among the largest known planets. Five of the seven systems have long-cadence observations by TESS which are included in the analysis. Of particular note is HAT-P-59 (TOI-1826.01) which is within the northern continuous viewing zone of the TESS mission, and HAT-P-60, which is the TESS candidate TOI-1580.01.

  PublisherOA PDFDOI

• Reprint of: Dating the Endometrial Biopsy

  Fertility and Sterility · 2019-10-01 · 295 citations

  article1st authorCorresponding
  PublisherDOI

• VizieR Online Data Catalog: Differential photometry & RVs of HAT-P-69 & HAT-P-70 (Zhou+, 2019)

  yCat · 2019-10-01

  article
  Publisher

• Two new HATNet hot Jupiters around A stars, and the first glimpse at the occurrence rate of hot Jupiters from TESS

  University of Southern Queensland ePrints (University of Southern Queensland) · 2019-06-02 · 99 citations

  articleOpen access

  Wide field surveys for transiting planets are well suited to searching diverse stellar populations, enabling a better understanding of the link between the properties of planets and their parent stars. We report the discovery of HAT-P-69b (TOI 625.01) and HAT-P-70b (TOI 624.01), two new hot Jupiters around A stars from the HATNet survey which have also been observed by the Transiting Exoplanet Survey Satellite (TESS). HAT-P-69b has a mass of 3.58 +0.58/-0.58 MJup and a radius of 1.676 +0.051/-0.033 RJup, residing in a prograde 4.79-day orbit. HAT-P-70b has a radius of 1.87 +0.15/-0.10 RJup and a mass constraint of < 6.78 (3 sigma) MJup, and resides in a retrograde 2.74-day orbit. We use the confirmation of these planets around relatively massive stars as an opportunity to explore the occurrence rate of hot Jupiters as a function of stellar mass. We define a sample of 47,126 main-sequence stars brighter than Tmag=10 that yields 31 giant planet candidates, including 18 confirmed planets, 3 candidates, and 10 false positives. We find a net hot Jupiter occurrence rate of 0.41+/-0.10 % within this sample, consistent with the rate measured by Kepler for FGK stars. When divided into stellar mass bins, we find the occurrence rate to be 0.71+/-0.31% for G stars, 0.43+/-0.15% for F stars, and 0.26+/-0.11% for A stars. Thus, at this point, we cannot discern any statistically significant trend in the occurrence of hot Jupiters with stellar mass.

  OA PDFDOI

• Velocity Fields in the Solar Atmosphere

  2018-05-11

  book-chapter

  Velocity fields in the solar atmosphere have been detected and measured by an adaptation of a technique previously used for measuring magnetic fields. Data obtained during the summers of 1960 and 1961 have been partially analyzed and yield the following principal results: 1. Large “cells” of horizontally moving material are distributed roughly uniformly over the entire solar surface. The motions within each cell suggest a (horizontal) outward flow from a source inside the cell. Typical diameters are 1.6 × 104 km; spacings between centers, 3 × 104 km (~5 × 103 cells over the solar surface); r.m.s. velocities of outflow, 0.5 km sec−1; lifetimes, 104 sec. There is a similarity in appearance to the Ca+ network. The appearance and properties of these cells suggest that they are a surface manifestation of a “supergranulation” pattern of convective currents which come from relatively great depths inside the sun. 2. A distinct correlation is observed between local brightness fluctuations and vertical velocities: bright elements tend to move upward, at the levels at which the lines Fe λ 6102 and Ca λ 6103 are formed. In the line Ca λ 6103, the correlation coefficient is ~0.5. This correlation appears to reverse in sign in the height range spanned by the Doppler wings of the Na D1 line and remains reversed at levels up to that of Ca+ λ 8542. At the level of Ca λ 6103, an estimate of the mechanical energy transport yields the rather large value 2 W cm−2. 3. The characteristic “cell size” of the vertical velocities appears to increase with height from ~1700 km at the level of Fe λ 6102 to ~3500 km at that of Na λ 5896. The r.m.s. vertical velocity of ~0.4 km sec−1 appears nearly constant over this height range. 4. The vertical velocities exhibit a striking repetitive time correlation, with a period T = 296 ± 3 sec. This quasi-sinusoidal motion has been followed for three full periods in the line Ca λ 6103, and is also clearly present in Fe λ 6102, Na λ 5896, and other lines. The energy contained in this oscillatory motion is about 160 J cm−2; the “losses” can apparently be compensated for by the energy transport (2). 5. A similar repetitive time correlation, with nearly the same period, seems to be present in the brightness fluctuations observed on ordinary spectroheliograms taken at the center of the Na D1 line. We believe that we are observing the transformation of potential energy into wave energy through the brightness-velocity correlation in the photosphere, the upward propagation of this energy by waves of rather well-defined frequency, and its dissipation into heat in the lower chromosphere. 6. Doppler velocities have been observed at various heights in the upper chromosphere by means of the Ha line. At great heights one finds a granular structure with a mean size of about 3600 km, but at lower levels one finds predominantly downward motions, which are concentrated in “tunnels” which presumably follow magnetic lines of force and are geometrically related to the Ca+ network. The Doppler field changes its appearance very rapidly at higher levels, typical lifetimes being about 30 seconds.

  PublisherDOI

• VizieR Online Data Catalog: HAT-TR-318-007: a double-lined M dwarf binary (Hartman+, 2018)

  VizieR Online Data Catalog · 2018-10-01

  article
  Publisher

• WHAT CAN OTHER STARS TELL US ABOUT THE SUN?

  University of Arizona Press eBooks · 2018-01-31 · 3 citations

  book-chapter1st authorCorresponding
  PublisherDOI

• VizieR Online Data Catalog: Differential photometry of the F-subgiant HAT-P-67 (Zhou+, 2017)

  yCat · 2018-04-01

  article
  Publisher

• HATS-22b, HATS-23b and HATS-24b: three new transiting super-Jupiters from the HATSouth project

  Monthly Notices of the Royal Astronomical Society · 2017-02-28 · 20 citations

  articleOpen access

  We report the discovery of three moderately high-mass transiting hot Jupiters from the HAT-South survey: HATS-22b, HATS-23b and HATS-24b. These planets add to the number of known planets in the 2M J regime. HATS-22b is a 2.74 0.11 M J mass and 0.953 +0.048 -0.029 R J radius planet orbiting a V = 13.455 0.040 sub-solar mass (M * = 0.759 0.019 M ; R * = 0.759 0.019 R ) K-dwarf host star on an eccentric (e = 0.079 0.026) orbit. This planet's high planet-to-stellar mass ratio is further evidence that migration mechanisms for hot Jupiters may rely on exciting orbital eccentricities that bring the planets closer to their parent stars followed by tidal circularization. HATS-23b is a 1.478 0.080 M J mass and 1.69 0.24 R J radius planet on a grazing orbit around a V = 13.901 0.010 G-dwarf with properties very similar to those of the Sun (M * = 1.115 0.054; R * = 1.145 0.070). HATS-24b orbits a moderately bright V = 12.830 0.010 F-dwarf star (M * = 1.218 0.036 M ; R = 1.194 +0.066 -0.041 R ). This planet has a mass of 2.39 +0.21 -0.12 M J and an inflated radius of 1.516 +0.085 -0.065 R J .

  PublisherOA PDFDOI

• HAT-P-67b: An Extremely Low Density Saturn Transiting an F-subgiant Confirmed via Doppler Tomography^∗

  The Astronomical Journal · 2017-04-13 · 48 citations

  articleOpen access

  Abstract We report the discovery of HAT-P-67b, which is a hot-Saturn transiting a rapidly rotating F-subgiant. HAT-P-67b has a radius of , and orbites a , host star in a ∼4.81 day period orbit. We place an upper limit on the mass of the planet via radial velocity measurements to be , and a lower limit of by limitations on Roche lobe overflow. Despite being a subgiant, the host star still exhibits relatively rapid rotation, with a projected rotational velocity of , which makes it difficult to precisely determine the mass of the planet using radial velocities. We validated HAT-P-67b via two Doppler tomographic detections of the planetary transit, which eliminate potential eclipsing binary blend scenarios. The Doppler tomographic observations also confirm that HAT-P-67b has an orbit that is aligned to within 12°, in projection, with the spin of its host star. HAT-P-67b receives strong UV irradiation and is among one of the lowest density planets known, which makes it a good candidate for future UV transit observations in the search for an extended hydrogen exosphere.

  PublisherDOI

Frequent coauthors

• G. Á. Bakos

  133 shared

• J. D. Hartman

  92 shared

• G. Kovács

  82 shared

• I. Papp

  Wigner Research Centre for Physics

  71 shared

• P. Sári

  Eötvös Loránd University

  70 shared

• J. Lázár

  University of Debrecen

  67 shared

• David W. Latham

  67 shared

• Geoffrey W. Marcy

  Health Awareness (United States)

  62 shared

Education

• Ph.D., Astronomy

  Harvard University

  1989

• B.A., Physics

  Harvard University

  1984