CaltechAUTHORS
  A Caltech Library Service

A Tendency Toward Alignment in Single-star Warm-Jupiter Systems

Rice, Malena and Wang, Songhu and Wang, Xian-Yu and Stefánsson, Guđmundur and Isaacson, Howard and Howard, Andrew W. and Logsdon, Sarah E. and Schweiker, Heidi and Dai, Fei and Brinkman, Casey and Giacalone, Steven and Holcomb, Rae (2022) A Tendency Toward Alignment in Single-star Warm-Jupiter Systems. Astronomical Journal, 164 (3). p. 104. ISSN 0004-6256. doi:10.3847/1538-3881/ac8153. https://resolver.caltech.edu/CaltechAUTHORS:20220829-468372700

Full text is not posted in this repository. Consult Related URLs below.

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20220829-468372700

Abstract

The distribution of spin–orbit angles for systems with wide-separation, tidally detached exoplanets offers a unique constraint on the prevalence of dynamically violent planetary evolution histories. Tidally detached planets provide a relatively unbiased view of the primordial stellar obliquity distribution, as they cannot tidally realign within the system lifetime. We present the third result from our Stellar Obliquities in Long-period Exoplanet Systems (SOLES) survey: a measurement of the Rossiter–McLaughlin effect across two transits of the tidally detached warm Jupiter TOI-1478 b with the WIYN/NEID and Keck/HIRES spectrographs, revealing a sky-projected spin–orbit angle λ = 6.2^(+5.9°)_(−5.5). Combining this new measurement with the full set of archival obliquity measurements, including two previous constraints from the SOLES survey, we demonstrate that, in single-star systems, tidally detached warm Jupiters are preferentially more aligned than closer-orbiting hot Jupiters. This finding has two key implications: (1) planets in single-star systems tend to form within aligned protoplanetary disks, and (2) warm Jupiters form more quiescently than hot Jupiters, which, in single-star systems, are likely perturbed into a misaligned state through planet–planet interactions in the post-disk-dispersal phase. We also find that lower-mass Saturns span a wide range of spin–orbit angles, suggesting a prevalence of planet–planet scattering and/or secular mechanisms in these systems.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-3881/ac8153DOIJournal Article
ORCID:
AuthorORCID
Rice, Malena0000-0002-7670-670X
Wang, Songhu0000-0002-7846-6981
Wang, Xian-Yu0000-0002-0376-6365
Stefánsson, Guđmundur0000-0001-7409-5688
Isaacson, Howard0000-0002-0531-1073
Howard, Andrew W.0000-0001-8638-0320
Logsdon, Sarah E.0000-0002-9632-9382
Schweiker, Heidi0000-0001-9580-4869
Dai, Fei0000-0002-8958-0683
Brinkman, Casey0000-0002-4480-310X
Giacalone, Steven0000-0002-8965-3969
Holcomb, Rae0000-0002-5034-9476
Additional Information:We thank our anonymous reviewer for their comments that have strengthened this manuscript. Over the duration of this project, M.R. was supported by the Heising–Simons Foundation 51 Pegasi b Fellowship and by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE-1752134. The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This work is supported by the Astronomical Big Data Joint Research Center, cofounded by the National Astronomical Observatories, Chinese Academy of Sciences, and Alibaba Cloud. This research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper contains data taken with the NEID instrument, which was funded by the NASA-NSF Exoplanet Observational Research (NN-EXPLORE) partnership and built by Pennsylvania State University. NEID is installed on the WIYN 3.5 m telescope at KPNO, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the NSF. The NEID archive is operated by the NASA Exoplanet Science Institute at the California Institute of Technology. We thank the NEID Queue Observers and WIYN Observing Associates for their skillful execution of our NEID observations. The authors are honored to be permitted to conduct astronomical research on Iolkam Du'ag (Kitt Peak), a mountain with particular significance to the Tohono O'odham. Facilities: Keck: I (HIRES) - , WIYN (NEID) - , Exoplanet Archive - , Extrasolar Planets Encyclopaedia - . Software: numpy (Oliphant 2006; Walt et al. 2011; Harris et al. 2020), matplotlib (Hunter 2007), pandas (McKinney et al. 2010), scipy (Virtanen et al. 2020), allesfitter (Günther & Daylan 2021), emcee (Foreman-Mackey et al. 2013), MESA (Paxton et al. 2010, 2013, 2015).
Group:Astronomy Department
Funders:
Funding AgencyGrant Number
National Science FoundationDGE-1752134
Heising–Simons Foundation 51 Pegasi b FellowshipUNSPECIFIED
Astronomical Big Data Joint Research CenterUNSPECIFIED
Keck Observatory Archive (KOA)UNSPECIFIED
NASA Exoplanet ArchiveUNSPECIFIED
Exoplanet Exploration ProgramUNSPECIFIED
NASA-NSF Exoplanet Observational Research (NN-EXPLORE)UNSPECIFIED
Issue or Number:3
DOI:10.3847/1538-3881/ac8153
Record Number:CaltechAUTHORS:20220829-468372700
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20220829-468372700
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:116625
Collection:CaltechAUTHORS
Deposited By: Donna Wrublewski
Deposited On:07 Sep 2022 22:24
Last Modified:07 Sep 2022 22:24

Repository Staff Only: item control page