First Detection of Submillimeter-wave [13C i] 3P1–3P0 Emission in a Gaseous Debris Disk of 49 Ceti with ALMA

Higuchi, Aya E.; Oya, Yoko; Yamamoto, Satoshi

doi:10.3847/2041-8213/ab518d

Cited by 7 publications

(4 citation statements)

References 24 publications

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“…For C 0 , the temperature of ∼24 K as well as the column density we derive are consistent with the results by Higuchi et al (2019a). The fact that T CO < T C might suggest that C and CO occupy different layers in the disk.…”

Section: B3 Temperature Priorsupporting

confidence: 91%

“…a Higuchi et al (2019a) derive a C I/ 13 C I peak intensity ratio of 12 ± 3. We assume that the same ratio applies to the disk-integrated fluxes.…”

Section: Alma Datamentioning

confidence: 94%

“…The edge-on, gas-rich debris disk around 49 Ceti has been the subject of multiple detailed studies over the past years (some of the more recent work includes Higuchi et al 2019aHiguchi et al , 2019bHiguchi et al , 2020Moór et al 2019;Pawellek et al 2019;Klusmeyer et al 2021). Hughes et al (2017) presented two non-LTE models of the CO disk around 49 Ceti with CO/H 2 abundances of 10 −4 (representing a primordial gas) and 1 (representing a secondary gas).…”

Section: Appendix a Continuum Fluxesmentioning

confidence: 99%

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Primordial or Secondary? Testing Models of Debris Disk Gas with ALMA*

Cataldi

Aikawa

Iwasaki

et al. 2023

ApJ

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The origin and evolution of gas in debris disks are still not well understood. Secondary gas production from cometary material or a primordial origin have been proposed. So far, observations have mostly concentrated on CO, with only a few C observations available. We overview the C and CO content of debris disk gas and test state-of-the-art models. We use new and archival Atacama Large Millimeter/submillimeter Array (ALMA) observations of CO and C i emission, complemented by C ii data from Herschel, for a sample of 14 debris disks. This expands the number of disks with ALMA measurements of both CO and C i by 10 disks. We present new detections of C i emission toward three disks: HD 21997, HD 121191, and HD 121617. We use a simple disk model to derive gas masses and column densities. We find that current state-of-the-art models of secondary gas production overpredict the C0 content of debris disk gas. This does not rule out a secondary origin, but might indicate that the models require an additional C removal process. Alternatively, the gas might be produced in transient events rather than a steady-state collisional cascade. We also test a primordial gas origin by comparing our results to a simplified thermochemical model. This yields promising results, but more detailed work is required before a conclusion can be reached. Our work demonstrates that the combination of C and CO data is a powerful tool to advance our understanding of debris disk gas.

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Section: B3 Temperature Priorsupporting

confidence: 91%

“…a Higuchi et al (2019a) derive a C I/ 13 C I peak intensity ratio of 12 ± 3. We assume that the same ratio applies to the disk-integrated fluxes.…”

Section: Alma Datamentioning

confidence: 94%

Section: Appendix a Continuum Fluxesmentioning

confidence: 99%

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Primordial or Secondary? Testing Models of Debris Disk Gas with ALMA*

Cataldi

Aikawa

Iwasaki

et al. 2023

ApJ

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“…An explanation is therefore needed for the more than 20 gaseous debris disks observed around stars older than 10 Myr (e.g., Kóspál et al 2013;Lieman-Sifry et al 2016;Marino et al 2016;Higuchi et al 2017;Hughes et al 2017;Moór et al 2017;Higuchi et al 2019aHiguchi et al , 2019bKral et al 2020). Two hypotheses have been proposed for the origins of this gas.…”

Section: Introductionmentioning

confidence: 99%

A Primordial Origin for the Gas-rich Debris Disks around Intermediate-mass Stars

Nakatani,

Turner,

Hasegawa

et al. 2023

ApJL

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While most debris disks consist of dust with little or no gas, a fraction have significant amounts of gas detected via emission lines of CO, ionized carbon, and/or atomic oxygen. Almost all such gaseous debris disks known are around A-type stars with ages up to 50 Myr. We show, using semianalytic disk evolution modeling, that this can be understood if the gaseous debris disks are remnant protoplanetary disks that have become depleted of small grains compared to the interstellar medium. Photoelectric heating by the A stars’ far-UV (FUV) radiation is then inefficient, while the stars’ extreme-UV (EUV) and X-ray emissions are weak owing to a lack of surface convective zones capable of driving magnetic activity. In this picture, it is relatively difficult for stars outside the range of spectral types from A through early B to have such long-lived gas disks. Less-massive stars have stronger magnetic activity in the chromosphere, transition region, and corona with resulting EUV and X-ray emission, while more-massive stars have photospheres hot enough to produce strong EUV radiation. In both cases, primordial disk gas is likely to photoevaporate well before 50 Myr. These results come from 0D disk evolution models where we incorporate internal accretion stresses, MHD winds, and photoevaporation by EUV and X-ray photons with luminosities that are functions of the stellar mass and age. A key issue this work leaves open is how some disks become depleted in small dust so that FUV photoevaporation slows. Candidates include the grains’ growth, settling, radial drift, radiation force, and incorporation into planetary systems.

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Solar System Physics for Exoplanet Research

Horner

Kane

Marshall

et al. 2020

PASP

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Over the past three decades, we have witnessed one of the great revolutions in our understanding of the cosmos—the dawn of the Exoplanet Era. Where once we knew of just one planetary system (the solar system), we now know of thousands, with new systems being announced on a weekly basis. Of the thousands of planetary systems we have found to date, however, there is only one that we can study up-close and personal—the solar system. In this review, we describe our current understanding of the solar system for the exoplanetary science community—with a focus on the processes thought to have shaped the system we see today. In section one, we introduce the solar system as a single well studied example of the many planetary systems now observed. In section two, we describe the solar system's small body populations as we know them today—from the two hundred and five known planetary satellites to the various populations of small bodies that serve as a reminder of the system's formation and early evolution. In section three, we consider our current knowledge of the solar system's planets, as physical bodies. In section four we discuss the research that has been carried out into the solar system's formation and evolution, with a focus on the information gleaned as a result of detailed studies of the system's small body populations. In section five, we discuss our current knowledge of planetary systems beyond our own—both in terms of the planets they host, and in terms of the debris that we observe orbiting their host stars. As we learn ever more about the diversity and ubiquity of other planetary systems, our solar system will remain the key touchstone that facilitates our understanding and modeling of those newly found systems, and we finish section five with a discussion of the future surveys that will further expand that knowledge.

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First Detection of Submillimeter-wave [¹³C i] ³P₁–³P₀ Emission in a Gaseous Debris Disk of 49 Ceti with ALMA

Cited by 7 publications

References 24 publications

Primordial or Secondary? Testing Models of Debris Disk Gas with ALMA*

Primordial or Secondary? Testing Models of Debris Disk Gas with ALMA*

A Primordial Origin for the Gas-rich Debris Disks around Intermediate-mass Stars

Solar System Physics for Exoplanet Research

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