Papers › TKS X: Confirmation of TOI-1444b and a Comparative Analysis of the Ultra-short-period...
TKS X: Confirmation of TOI-1444b and a Comparative Analysis of the Ultra-short-period Planets with Hot Neptunes
Fei Dai, Andrew W. Howard, Natalie M. Batalha, Corey Beard, Aida Behmard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Ian J. M. Crossfield, Paul A. Dalba, Courtney Dressing, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Daniel Huber, Howard Isaacson, Stephen R. Kane, Jack Lubin, Andrew Mayo, Teo Mocnik, Joseph M. Akana Murphy, Erik A. Petigura, Malena Rice, Paul Robertson, Lee Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Judah Van Zandt, Charles Beichman, David Ciardi, Karen A. Collins, Erica Gonzales, Steve B. Howell, Rachel A. Matson, Elisabeth C. Matthews, Joshua E. Schlieder, Richard P. Schwarz, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Douglas A. Caldwell, Knicole D. Colon, Diana Dragomir, Michael B. Lund, Brian McLean, Alexander Rudat, Avi Shporer
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We report the discovery of TOI-1444b, a 1.4-R_⊕ super-Earth on a 0.47-day orbit around a Sun-like star discovered by {\it TESS}. Precise radial velocities from Keck/HIRES confirmed the planet and constrained the mass to be 3.87 ±0.71 M_⊕. The RV dataset also indicates a possible non-transiting, 16-day planet (11.8±2.9M_⊕). We report a tentative detection of phase curve variation and secondary eclipse of TOI-1444b in the {\it TESS} bandpass. TOI-1444b joins the growing sample of 17 ultra-short-period planets with well-measured masses and sizes, most of which are compatible with an Earth-like composition. We take this opportunity to examine the expanding sample of ultra-short-period planets (<2R_⊕) and contrast them with the newly discovered sub-day ultra-hot Neptunes (>3R_⊕, >2000F_⊕ TOI-849 b, LTT9779 b and K2-100). We find that 1) USPs have predominately Earth-like compositions with inferred iron core mass fractions of 0.32±0.04; and have masses below the threshold of runaway accretion (∼10M_⊕), while ultra-hot Neptunes are above the threshold and have H/He or other volatile envelope. 2) USPs are almost always found in multi-planet system consistent with a secular interaction formation scenario; ultra-hot Neptunes (P_(orb) ≲1 day) tend to be ``lonely' similar to longer-period hot Neptunes(P_(orb)1-10 days) and hot Jupiters. 3) USPs occur around solar-metallicity stars while hot Neptunes prefer higher metallicity hosts. 4) In all these respects, the ultra-hot Neptunes show more resemblance to hot Jupiters than the smaller USP planets, although ultra-hot Neptunes are rarer than both USP and hot Jupiters by 1-2 orders of magnitude.
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