---
title: 'TOI-1743 b: A Transiting Super-Earth'
url: https://www.emergentmind.com/topics/toi-1743-b
type: topic
---

# TOI-1743 b: A Transiting Super-Earth

TOI-1743 b is a transiting super-Earth exoplanet orbiting an early M-dwarf (spectral type M4V), discovered by the Transiting Exoplanet Survey Satellite (TESS). Identified as one of several planets in a cohort of super-Earth to Neptune-sized planets around M dwarfs, TOI-1743 b features well-constrained physical and orbital parameters and occupies a significant position within the so-called radius valley—a region in parameter space that is integral to studies of planetary formation and atmospheric evolution.

## 1. Discovery and Photometric Detection

TOI-1743 b was detected by the TESS mission as a periodic transit signature in high-cadence (2-minute) light curves spanning up to 39 observational sectors. The shape, depth, and recurrence of the signal indicated a transiting planetary companion. The initial detection in TESS data was corroborated and refined via subsequent ground-based photometric campaigns, employing multiple facilities including TUG-T100, SAINT-EX, TRAPPIST-North, LCOGT, KeplerCam, and MuSCAT3. The joint approach allowed for increased temporal coverage, independent verification of ephemerides, and scrutiny of possible astrophysical false positives [2509.05038].

## 2. Planetary Signal Validation

The validation process of TOI-1743 b combined several robust methodologies:

- Analysis of TESS Data Validation (DV) reports, including odd–even transit depth comparison, centroid motion checks, "ghost" contamination tests, and bootstrap resampling, all confirmed the integrity of the transit signal.
- High-resolution imaging (both optical speckle and adaptive optics) supplemented by archival images was conducted to exclude unresolved background or gravitationally bound stellar companions capable of producing a transit-like signal.
- A statistical validation was performed using TRICERATOPS, which delivered an exceptionally low false positive probability (FPP) of
  $$
  \mathrm{FPP} = (2.996 \pm 1.910) \times 10^{-5},
  $$
  strongly confirming the planetary nature.
- Spectroscopic reconnaissance with, for example, the Shane/Kast spectrograph, further supported stellar classification and simultaneously excluded close eclipsing binaries.

## 3. Physical and Orbital Characteristics

Table 1 summarizes the principal measured parameters for TOI-1743 b as determined through a joint analysis (via EXOFASTv2) of TESS and ground-based photometric datasets:

| Parameter               | Value                                    | Uncertainty                |
|-------------------------|------------------------------------------|----------------------------|
| Orbital period ($P$)    | $4.266046$ days                          | $\pm 0.000002$ days        |
| Planetary radius ($R_p$)| $1.83\;R_\oplus$                         | $+0.11/-0.10\;R_\oplus$    |
| Equilibrium temperature ($T_{\rm eq}$) | $485\;\mathrm{K}$      | $+14 / -13\;\mathrm{K}$    |
| Transit depth $(R_p/R_\star)^2$ | $\approx 0.0496$                 | (dimensionless)            |

These values place TOI-1743 b in the small-radius, short-period regime typical for rocky super-Earths orbiting M dwarfs. The transit depth quantifies the fraction of stellar flux occulted and is consistent with the derived stellar and planetary radii.

## 4. Context: The Radius Valley and Planetary Structure

TOI-1743 b occupies a locus in the radius–period parameter space known as the radius valley. This regime is characterized by a paucity of sub-Neptunes and is interpreted as marking the transition between planets with substantial hydrogen–helium envelopes and those that are primarily rocky (super-Earths). For low-mass stars, such as M dwarfs, this feature serves as an empirical constraint on atmospheric loss mechanisms (e.g., photoevaporation, core-powered mass loss).

With a measured radius of $1.83~R_\oplus$, TOI-1743 b aligns with the lower-radius, likely rocky population within the bimodal distribution. This status is of specific value for testing atmospheric evolution models and determining the boundary conditions governing volatile retention.

## 5. Prospects for Mass Measurement and Atmospheric Characterization

TOI-1743 b is suitable for both radial velocity (RV) follow-up and atmospheric studies, owing to the host star’s near-infrared brightness ($K_{mag} < 11$) and the planet’s orbital and physical characteristics. The expected RV semi-amplitude is
$$
K_\star \approx 3.7^{+1.4}_{-0.9}\; \mathrm{m/s},
$$
which is accessible via current near-infrared spectrographs. Consequently, precise mass determination is feasible.

The planet’s Transmission Spectroscopy Metric (TSM), approximately $60 \pm 25$, indicates favorable prospects for atmospheric exploration via platforms such as JWST. Atmospheric models suggest that if a significant volatile envelope exists, molecular absorption features (H\(_2\)O, CH\(_4\), CO\(_2\)) should be detectable at typical spectroscopic signal-to-noise ratios. Achieving precise mass and radius measurements will reduce degeneracies in compositional modeling, further informing the study of planetary evolution in the radius valley.

## 6. Implications for Planet Formation and Comparative Exoplanetology

TOI-1743 b, along with comparably validated super-Earths (e.g., TOI-5799 b and TOI-5799 c), provides a laboratory for empirical examination of planet formation pathways in M-dwarf systems. Its well-constrained parameters and position within the radius valley facilitate critical tests of atmospheric loss and retention mechanisms. Continuous follow-up—combining RV, transit timing, and transmission or emission spectroscopy—will refine estimates of composition, bulk density, and atmospheric scale height, contributing directly to the statistical framework surrounding the origins of short-period rocky planets.

Source: https://www.emergentmind.com/topics/toi-1743-b